CDAWeb Served Heliophysics Datasets Beginning with 'W'
- WILD2_HELIO1HR_POSITION: Position in heliocentric coordinates from SPDF Helioweb - Natalia Papitashvili (NASA/GSFC/SPDF)
- WIND_3DP_ECHSFITS_E0-YR: Wind spacecraft, 3DP accurate electron parameters - Chadi S. Salem (University of California, Berkeley)
- WIND_3DP_L3-EESALOW-MOMENTS: A Three-Dimensional Plasma and Energetic particle investigation for the Wind spacecraft - L.B. Wilson III (NASA/GSFC)
- WIND_HELIO1HR_POSITION: Position in heliocentric coordinates from SPDF Helioweb - Natalia Papitashvili (NASA/GSFC/SPDF)
- WIND_WAVES_QTNFIT: WIND Radio/Plasma Wave, (WAVES) Quasi-Thermal Noise Key Parameters - Keith Goetz (University of Minnesota)
- WIND_WAVES_QTNFIT-FILTERED: WIND Radio/Plasma Wave, (WAVES) Filtered Quasi-Thermal Noise Key Parameters - Keith Goetz (University of Minnesota)
- WI_AT_DEF: Wind Definitive Attitude
- WI_AT_PRE: Wind Predicted Attitude
- WI_EHPD_3DP: Electron energy-angle distributions 100 eV - 30 keV, often at 24 sec, EESA High, Wind 3DP - R. Lin/S. Bale (UC Berkeley)
- WI_EHSP_3DP: Electron omnidirectional fluxes 100 eV-30 keV, often at 24 sec, EESA High, Wind 3DP - R. Lin/S. Bale (UC Berkeley)
- WI_ELM2_3DP: Electron Moments (ground-computed), EESA Low, Wind 3DP - R. Lin/S. Bale (UC Berkeley)
- WI_ELPD_3DP: Electron energy-angle distributions 5-1100 eV, often at 24 sec, EESA Low, Wind 3DP - R. Lin/S. Bale (UC Berkeley)
- WI_ELSP_3DP: Electron omnidirectional fluxes 5-1100 eV, often at 24 sec, EESA Low, Wind 3DP - R. Lin/S. Bale (UC Berkeley)
- WI_EMFITS_E0_3DP: Wind spacecraft, 3DP electron moments - Stuart D. Bale (University of California, Berkeley)
- WI_EM_3DP: Electron Plasma moments (computed on-board) (NOT CORRECTED FOR S/C POTENTIAL) @ 3 second (spin) resolution (version 3), EESA LOW, Wind 3DP - R. Lin/S. Bale (UC Berkeley)
- WI_EPACT_STEP-DIFFERENTIAL-ION-FLUX-1HR: Wind EPACT-STEP - Mihir Desai (University of Texas, San Antonio)
- WI_EPACT_STEP-DIRECTIONAL-DIFF-CNO-FLUX-10MIN: Wind EPACT-STEP CNO - Mihir Desai (University of Texas, San Antonio)
- WI_EPACT_STEP-DIRECTIONAL-DIFF-FE-FLUX-10MIN: Wind EPACT-STEP FE - Mihir Desai (University of Texas, San Antonio)
- WI_EPACT_STEP-DIRECTIONAL-DIFF-H-FLUX-10MIN: Wind EPACT-STEP H - Mihir Desai (University of Texas, San Antonio)
- WI_EPACT_STEP-DIRECTIONAL-DIFF-HE-FLUX-10MIN: Wind EPACT-STEP HE - Mihir Desai (University of Texas, San Antonio)
- WI_H0_MFI: Wind Magnetic Fields Investigation: 3 sec, 1 min, and hourly Definitive Data. - A. Koval (UMBC, NASA/GSFC)
- WI_H0_SWE: Wind SOLAR WIND EXPERIMENT 6 - 12 sec solar wind electron moments - K. Ogilvie (GSFC Code 692)
- WI_H0_WAV: WIND Radio/Plasma Wave, (WAVES) Key Parameters - M. L. Kaiser (GSFC)
- WI_H1_SWE: Solar wind proton and alpha parameters, including anisotropic temperatures, derived by non-linear fitting of the measurements and with moment techniques. - Keith W. Ogilvie (NASA GSFC)
- WI_H1_SWE_RTN: Solar wind proton and alpha parameters, including anisotropic temperatures, derived by non-linear fitting of the measurements and with moment techniques. Data in RTN - Bennett Maruca (University of Delaware)
- WI_H1_WAV: Wind Radio/Plasma Wave, (WAVES) Hi-Res Parameters - M. L. Kaiser (GSFC)
- WI_H2_MFI: Wind Magnetic Fields Investigation, High-resolution Definitive Data - A. Koval (UMBC, NASA/GSFC)
- WI_H3-RTN_MFI: Wind Magnetic Fields Investigation: 3 sec, 1 min, and hourly Definitive Data (RTN). - A. Koval (UMBC, NASA/GSFC)
- WI_H3_SWE: Wind SOLAR WIND EXPERIMENT 9 sec solar wind electron pitch-angle distributions - K. Ogilvie (NASA/GSFC)
- WI_H4-RTN_MFI: Wind Magnetic Fields Investigation, High-resolution Definitive Data (RTN) - A. Koval (UMBC, NASA/GSFC)
- WI_H4_SWE: 3 sec solar wind electron pitch-angle distributions at 6-12 sec cadence, Wind Solar Wind Experiment (SWE) - K. Ogilvie (NASA/GSFC)
- WI_H5_SWE: Wind SOLAR WIND EXPERIMENT 9 sec solar wind electron moments - K. Ogilvie (NASA/GSFC)
- WI_K0_3DP: Wind 3-D Plasma Analyzer, Key Parameters [PRELIM] - R. Lin/S. Bale (UC Berkeley)
- WI_K0_EPA: Wind Energetic Particle Acceleration Composition Transport, Key Parameters [PRELIM] - T. Von Roseavinge (NASA/GSFC)
- WI_K0_GIFWALK: Links to Wind KP pre-generated survey and other plots - Polar-Wind-Geotail Ground System (NASA GSFC)
- WI_K0_MFI: Wind Magnetic Fields Investigation, Key Parameters - R. Lepping (NASA/GSFC)
- WI_K0_SMS: Solar Wind and Suprathermal Ion Composition Instrument, Key Parameters - G. Gloeckler (U of MD Maryland)
- WI_K0_SPHA: Wind Spin Phase
- WI_K0_SWE: Wind Solar Wind Experiment, Key Parameters - K. Ogilvie (NASA GSFC)
- WI_K0_SWE_RTN: Wind Solar Wind Experiment, Key Parameters in RTN - Bennett Maruca (University of Delaware)
- WI_K0_WAV: WIND Radio/Plasma Wave, (WAVES) Key Parameters - M. L. Kaiser (GSFC)
- WI_K1-RTN_MFI: Wind Magnetic Fields Investigation, Key Parameters in RTN - Andriy Koval (UMBC)
- WI_L2-1HOUR-SEP_EPACT-APE_B: Wind EPACT-APE_B H 18.90 -21.90 MeV Solar Energetic Particle Intensities, 1-Hour Level 2 Data - T. Von Rosenvinge & D. Reames (NASA GSFC)
- WI_L2-1HOUR-SEP_EPACT-LEMT: Wind EPACT-LEMT He/C/O/Ne/Si/Fe 2-11 MeV/Nuc Solar Energetic Particle Intensities, 1-Hour Level 2 Data - T. Von Rosenvinge & D. Reames (NASA GSFC)
- WI_L2-30MIN_SMS-STICS-AFM-MAGNETOSPHERE: Solar Wind and Suprathermal Ion Composition Instrument, Key Parameters - S. T. Lepri (U of Michigan)
- WI_L2-30MIN_SMS-STICS-AFM-SOLARWIND: Solar Wind and Suprathermal Ion Composition Instrument, Key Parameters - S. T. Lepri (U of Michigan)
- WI_L2-30MIN_SMS-STICS-ERPA-MAGNETOSPHERE: Magnetosphere and Suprathermal Ion Composition Instrument, Key Parameters - S. T. Lepri (U of Michigan)
- WI_L2-30MIN_SMS-STICS-ERPA-SOLARWIND: Solar Wind and Suprathermal Ion Composition Instrument, Key Parameters - S. T. Lepri (U of Michigan)
- WI_L2-3MIN_SMS-STICS-VDF-MAGNETOSPHERE: Magnetosphere and Suprathermal Ion Composition Instrument, Key Parameters - S. T. Lepri (U of Michigan)
- WI_L2-3MIN_SMS-STICS-VDF-SOLARWIND: Solar Wind and Suprathermal Ion Composition Instrument, Key Parameters - S. T. Lepri (U of Michigan)
- WI_L2-5MIN-SEP_EPACT-LEMT: Wind EPACT-LEMT He/C/O/Ne/Si/Fe 2-11 MeV/Nuc Solar Energetic Particle Intensities, 5min Level 2 Data - T. Von Rosenvinge & D. Reames (NASA GSFC)
- WI_L2_3MIN_SMS-STICS-NVT-MAGNETOSPHERE: Solar Wind and Suprathermal Ion Composition Instrument, Key Parameters - S. T. Lepri (U of Michigan)
- WI_L2_3MIN_SMS-STICS-NVT-SOLARWIND: Solar Wind and Suprathermal Ion Composition Instrument, Key Parameters - S. T. Lepri (U of Michigan)
- WI_L2_WAV_RAD1: Wind/WAVES/RAD1 Data - Karine Issautier (Karine.Issautier@obspm.fr) (LESIA, Observatoire de Paris-PSL, CNRS)
- WI_L2_WAV_RAD2: Wind/WAVES/RAD2 Data - Karine Issautier (Karine.Issautier@obspm.fr) (LESIA, Observatoire de Paris-PSL, CNRS)
- WI_L2_WAV_TNR: Wind/WAVES/TNR Data - Karine Issautier (Karine.Issautier@obspm.fr) (LIRA, Observatoire de Paris-PSL, CNRS)
- WI_L3-DUSTIMPACT_WAVES: The Radio and Plasma Wave Investigation on the Wind Spacecraft - D.M. Malaspina (U. Colorado at Boulder, LASP)
- WI_M0_SWE: Wind SOLAR WIND EXPERIMENT 9 sec solar wind electron pitch-angle distribution averages - K. Ogilvie (NASA/GSFC)
- WI_M2_SWE: Wind SOLAR WIND EXPERIMENT 3 sec solar wind electron pitch-angle distribution averages - K. Ogilvie (NASA/GSFC)
- WI_OR_DEF: Wind Definitive Orbit
- WI_OR_GIFWALK: Links to Wind and multi-mission orbit plots - Polar-Wind-Geotail Ground System (NASA GSFC)
- WI_OR_PRE: Wind Predicted Orbit
- WI_PLSP_3DP: Ion omnidirectional fluxes 0.4-3 keV and moments, often at ~24 second resolution, PESA Low, Wind 3DP - R. Lin/S. Bale (UC Berkeley)
- WI_PM_3DP: Ion moments (computed on-board) @ 3 second (spin) resolution, PESA LOW, Wind 3DP - R. Lin/S. Bale (UC Berkeley)
- WI_SFPD_3DP: Electron energy-angle distributions 27 keV to 520 keV, often at 24 sec, SST Foil, Wind 3DP - R. Lin/S. Bale (UC Berkeley)
- WI_SFSP_3DP: Electron omnidirectional fluxes 27 keV - 520 keV, often at 24 sec, SST Foil, Wind 3DP - R. Lin/S. Bale (UC Berkeley)
- WI_SOPD_3DP: Proton energy-angle distributions 70 keV - 6.8 MeV, often at 24 sec, SST Open, Wind 3DP - R. Lin/S. Bale (UC Berkeley)
- WI_SOSP_3DP: Proton omnidirectional fluxes 70 keV - 6.8 MeV, often at 24 sec, SST Open, Wind 3DP - R. Lin/S. Bale (UC Berkeley)
- WI_STRAHL0_SWE: Wind Solar Wind Experiment (SWE) strahl detector, ~1/2 sec solar wind electron pitch-angle distributions at ~12 sec cadence - K. Ogilvie (NASA/GSFC)
- WI_SW-ION-DIST_SWE-FARADAY: Faraday Cup orientation and charge flux - Keith Ogilvie (NASA GSFC)
- WI_WA_RAD1_L3_DF: Wind Waves, Level 3 Direction-Finding (DF) parameters - K. Issautier (LESIA, Observatoire de Paris-PSL, CNRS)
- Data Variable Descriptions
- Distance from Sun to object [RAD_AU]
- Latitude in Solar Ecliptic Coordinate System (SE) [SE_LAT]
- Longitude in Solar Ecliptic Coordinate System (SE) [SE_LON]
- Latitude in heliographic Rotating Coordinate System (HG) [HG_LAT]
- Longitude in Heliographic Rotating Coordinate System (HG) [HG_LON]
- Latitude in heliographic Inertial Coordinate System (HGI) [HGI_LAT]
- Longitude in heliographic Inertial Coordinate System (HGI) [HGI_LON]
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- WIND_3DP_ECHSFITS_E0-YR doi:10.48322/nbzq-1w25
- Description
These electron core halo and strahl parameters are moments of Wind 3DP EESA-L and EESA-H measurements, corrected for spacecraft potential and other instrumental effects. More information can be found at: C. S. Salem et al., Precision Electron Measurements in the Solar Wind at 1AU from NASA’s Wind spacecraft, Astron. & Astrophys., 2023. M. Pulupa et al., Spin-modulated spacecraft floating potential: Observations and effects on electron moments, J. Geophys. Res. Space Physics, Vol. 119, 647-657, doi:10.1002/2013JA019359, 2014. R. P. Lin et al., A Three-dimensional plasma and energetic particle investigation for the Wind spacecraft, Space Science Reviews, Vol. 71, p125-153, 1995.
- Data Variable Descriptions
- Total electron density moment in units of /cm^3 [N_e_dens_wi_3dp]
Total electron density moment from EESA-L and EESA-H
- Parallel total electron temperature moment in units of eV [T_e_par_wi_3dp]
Includes EESA-L and EESA-H data
- Perpendicular total electron temperature moment in units of eV [T_e_perp_wi_3dp]
Includes EESA-L and EESA-H data
- Parallel electron heat flux moment in units of uW/m^2 [Q_e_par_wi_3dp]
Includes EESA-L and EESA-H data
- Electron velocity vector moment in GSE coordinates in units of km/s [V_e_xyz_gse_wi_3dp]
Includes EESA-L and EESA-H data
- Electron Core density moment in units of /cm^3 [N_c_dens_wi_3dp]
Electron Core density moment from EESA-L and EESA-H
- Parallel Electron Core temperature moment in units of eV [T_c_par_wi_3dp]
Includes EESA-L and EESA-H data
- Perpendicular electron core temperature moment in units of eV [T_c_perp_wi_3dp]
Includes EESA-L and EESA-H data
- Parallel electron core drift velocity in the ion frame in units of km/s [Vd_c_par_wi_3dp]
Includes EESA-L and EESA-H data
- Electron halo density moment in units of /cm^3 [N_h_dens_wi_3dp]
Electron halo density moment from EESA-L and EESA-H
- Parallel Electron Core temperature moment in units of eV [T_h_par_wi_3dp]
Includes EESA-L and EESA-H data
- Perpendicular electron halo temperature moment in units of eV [T_h_perp_wi_3dp]
Includes EESA-L and EESA-H data
- Parallel electron halo drift velocity in the ion frame in units of km/s [Vd_h_par_wi_3dp]
Includes EESA-L and EESA-H data
- Electron strahl density moment in units of /cm^3 [N_s_dens_wi_3dp]
Electron strahl density moment from EESA-L and EESA-H
- Parallel Electron strahl temperature moment in units of eV [T_s_par_wi_3dp]
Includes EESA-L and EESA-H data
- Perpendicular electron strahl temperature moment in units of eV [T_s_perp_wi_3dp]
Includes EESA-L and EESA-H data
- Parallel electron strahl drift velocity in the ion frame in units of km/s [Vd_s_par_wi_3dp]
Includes EESA-L and EESA-H data
- Q, Quality parameter for electron data. It is calculated from the properties of the input data and goodness-of-fit statistics from the nonlinear fitting process. It varies between 0 and 10. Higher values of Q represent more confidence in the resulting electron parameters [Quality_wi_3dp]
Q is a quality parameter calculated from the properties of the input data and goodness-of-fit statistics from the nonlinear fitting process. It varies between 0 and 10. Higher values of Q represent more confidence in the resulting electron parameters
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- WIND_3DP_L3-EESALOW-MOMENTS
- Description
BAD for Q_FLAG = (V_oe,x GE -50 km/s) OR (|qe//|/qeo GE 1) OR (T_e,j LE 1 eV) GOOD for Q_FLAG = (V_oe,x LT -50 km/s) AND (|qe//|/qeo LT 1) AND (T_e,j GT 1 eV) The definition of GOOD and BAD derive from physically meaningful constraints as follows: Values of V_oe,x above -50 km/s start to imply possible sunward electron flow in the spacecraft frame, which is not physical Values of |qe//|/qeo at or above unity makes no physical sense since qeo is the free-streaming maximum limit Values of T_e,j at or below 1 eV are not meaningful as the instrument cannot measure such cold distributions
- Data Variable Descriptions
- Quality Flag of VDF velocity moments [Q_FLAG]
Quality flag of electron VDF velocity moments [1 = best, 8 = worst/do not use]
- Magnetic field vector [GSE] at time of VDF [B3_GSE]
Magnetic field 3-vector [nT, GSE] interpolated to time of 3DP VDF
- Spacecraft floating electric potential [PHI_SC]
Spacecraft potential [eV] at time of 3DP VDF
- Total electron density from upper hybrid line [NE_WAV]
Total electron number density [cm^(-3)] derived from neural network software used on the WAVES TNR data
- Total electron density from zeroth velocity moment of 3DP [NE_3DP]
Total electron number density [cm^(-3)] from zeroth velocity moment
- Uncertainty for NE_3DP from f - df [DNE3DL]
- Uncertainty for NE_3DP from f + df [DNE3DU]
- Electron bulk flow velocity from first velocity moment of 3DP [UE_3DP]
Electron bulk flow velocity [km/s, GSE] from first velocity moment
- Uncertainty for UE_3DP from f - df [DUE3DL]
- Uncertainty for UE_3DP from f + df [DUE3DU]
- Total electron thermal pressure from second velocity moment of 3DP [PS_3DP]
Scalar electron thermal pressure [eV cm^(-3)] from second velocity moment
- Uncertainty for PE_3DP from f - df [DPS3DL]
- Uncertainty for PE_3DP from f + df [DPS3DU]
- Electron temperatures from second velocity moment of 3DP [TE_3DP]
Electron temperatures [eV, FAC {para,perp, tot}] from second velocity moment- Uncertainty for TE_3DP from f - df [DTE3DL]
- Uncertainty for TE_3DP from f + df [DTE3DU]
- Electron temperature anisotropies from second velocity moment of 3DP [AE_3DP]
Electron temperature anisotropies [N/A, scalar] from second velocity moment
- Uncertainty for AE_3DP from f - df [DAE3DL]
- Uncertainty for AE_3DP from f + df [DAE3DU]
- Electron heat flux vector from third velocity moment of 3DP [QE_3DP]
Electron heat flux 3-vector [microW m^(-2), FAC {perp1,perp2,para}] from third velocity moment- Uncertainty for QE_3DP from f - df [DQE3DL]
- Uncertainty for QE_3DP from f + df [DQE3DU]
- Normalized electron heat flux vector from third velocity moment of 3DP [QN_3DP]
Normalized electron heat flux 3-vector [N/A, FAC {perp1,perp2,para}] from third velocity moment- Uncertainty for QN_3DP from f - df [DQN3DL]
- Uncertainty for QN_3DP from f + df [DQN3DU]
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-
WIND_HELIO1HR_POSITION doi:10.48322/90ar-hx32
Proper citations should include the "Accessed on date" in the form . - Description
No TEXT global attribute value.
- Data Variable Descriptions
- Distance from Sun to object [RAD_AU]
- Latitude in Solar Ecliptic Coordinate System (SE) [SE_LAT]
- Longitude in Solar Ecliptic Coordinate System (SE) [SE_LON]
- Latitude in heliographic Rotating Coordinate System (HG) [HG_LAT]
- Longitude in Heliographic Rotating Coordinate System (HG) [HG_LON]
- Latitude in heliographic Inertial Coordinate System (HGI) [HGI_LAT]
- Longitude in heliographic Inertial Coordinate System (HGI) [HGI_LON]
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- WIND_WAVES_QTNFIT
- Description
SSR WAVES: The Radio and Plasma Wave Investigation on the WIND Spacecraft, Vol 71, pg 231-263, 1995. JGRA: Solar Wind Electron Parameters Determination on Wind Spacecraft Using Quasi Thermal Noise Spectroscopy, Vol 125, JA028113 Variable note: suprathermal parameters (fit_a, delta_a, coarse_a, fit_t, delta_t, coarse_t), have large uncertainties due to instruemntal limitations. Commonly, for science purposes, medians on a scale of 1-5 minutes should be used.
- Data Variable Descriptions
- Electron number density from fits of selected QTN data [fit_n_e]
High resolution plasma densities: resolution depends on instrument mode and may vary.
- Electron number density uncertainty from fits of selected QTN data [delta_n_e]
High resolution plasma densities: resolution depends on instrument mode and may vary.
- Electron number density from plasma resonance peak [coarse_n_e]
High resolution plasma densities: resolution depends on instrument mode and may vary.
- Electron core temperature from fits of selected QTN data [fit_T_c]
High resolution plasma temperatures: resolution depends on instrument mode and may vary.
- Electron core temperature uncertainty from fits of selected QTN data [delta_T_c]
High resolution plasma temperatures: resolution depends on instrument mode and may vary.
- Electron core temperature from thermal plateau levels [coarse_T_c]
High resolution plasma temperatures: resolution depends on instrument mode and may vary.
- Halo to core electron density ratio from fits of selected QTN data [fit_a]
High resolution halo to core electron densities: resolution depends on instrument mode and may vary. For science purposes, using median values on a scale of 1-5 minutes is recommended.
- Halo to core electron density ratio uncertainty from fits of selected QTN data [delta_a]
High resolution halo to core electron densities: resolution depends on instrument mode and may vary. For science purposes, using median values on a scale of 1-5 minutes is recommended.
- Halo to core electron density ratio from fit initial guess [coarse_a]
High resolution halo to core electron densities: resolution depends on instrument mode and may vary. For science purposes, using median values on a scale of 1-5 minutes is recommended.
- Halo to core electron temperature ratio from fits of selected QTN data [fit_t]
High resolution halo to core electron temperatures: resolution depends on instrument mode and may vary. For science purposes, using median values on a scale of 1-5 minutes is recommended.
- Halo to core electron temperature ratio uncertainty from fits of selected QTN data [delta_t]
High resolution halo to core electron temperatures: resolution depends on instrument mode and may vary. For science purposes, using median values on a scale of 1-5 minutes is recommended.
- Halo to core electron temperature ratio from fit initial guess [coarse_t]
High resolution halo to core electron temperatures: resolution depends on instrument mode and may vary. For science purposes, using median values on a scale of 1-5 minutes is recommended.
- Quality Flag of QTN fits of selected QTN data [QF]
Quality flags for fits of high resolution data: resolution depends on instrument mode and may vary. This variable is a weighted sum of other QF, calculated as QF = 5*QF_points + 3*QF_peak + QF_shift + QF_low_level, with maximum realistic value of 10. QF > 2 is considered good quality. QF > 5 is considered highly reliable.
- Quality Flag of QTN fits of selected QTN data; from number of selected QTN channels [QF_points]
Quality flags for fits of high resolution data: resolution depends on instrument mode and may vary. Normalized between 0 and 1.
- Quality Flag of QTN fits of selected QTN data; from fitting the plasma peak [QF_peak]
Quality flags for fits of high resolution data: resolution depends on instrument mode and may vary. Normalized between 0 and 1, although can rarely take values above 1.
- Quality Flag of QTN fits of selected QTN data; from shifts between fit and data [QF_shift]
Quality flags for fits of high resolution data: resolution depends on instrument mode and may vary. Normalized between 0 and 1.
- Quality Flag of QTN fits of selected QTN data; from data levels lower then the fit [QF_low_level]
Quality flags for fits of high resolution data: resolution depends on instrument mode and may vary. Normalized between 0 and 1.
- Filtered data for quick survey use (outliers labeled). [filtered]
Intervals seleceted for quick statistical survey usage (0 - filtered out; 1 - good for survey use). User is recomended to ignore the filter and use QFs for detailed examination of particular events.
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- WIND_WAVES_QTNFIT-FILTERED
- Description
SSR WAVES: The Radio and Plasma Wave Investigation on the WIND Spacecraft, Vol 71, pg 231-263, 1995. JGRA: Solar Wind Electron Parameters Determination on Wind Spacecraft Using Quasi Thermal Noise Spectroscopy, Vol 125, JA028113 Variable note: suprathermal parameters (fit_a, delta_a, coarse_a, fit_t, delta_t, coarse_t), have large uncertainties due to instruemntal limitations. Commonly, for science purposes, medians on a scale of 1-5 minutes should be used.
- Data Variable Descriptions
- Electron number density from fits of selected QTN data [fit_n_e]
High resolution plasma densities: resolution depends on instrument mode and may vary.
- Electron number density uncertainty from fits of selected QTN data [delta_n_e]
High resolution plasma densities: resolution depends on instrument mode and may vary.
- Electron number density from plasma resonance peak [coarse_n_e]
High resolution plasma densities: resolution depends on instrument mode and may vary.
- Electron core temperature from fits of selected QTN data [fit_T_c]
High resolution plasma temperatures: resolution depends on instrument mode and may vary.
- Electron core temperature uncertainty from fits of selected QTN data [delta_T_c]
High resolution plasma temperatures: resolution depends on instrument mode and may vary.
- Electron core temperature from thermal plateau levels [coarse_T_c]
High resolution plasma temperatures: resolution depends on instrument mode and may vary.
- Halo to core electron density ratio from fits of selected QTN data [fit_a]
High resolution halo to core electron densities: resolution depends on instrument mode and may vary. For science purposes, using median values on a scale of 1-5 minutes is recommended.
- Halo to core electron density ratio uncertainty from fits of selected QTN data [delta_a]
High resolution halo to core electron densities: resolution depends on instrument mode and may vary. For science purposes, using median values on a scale of 1-5 minutes is recommended.
- Halo to core electron density ratio from fit initial guess [coarse_a]
High resolution halo to core electron densities: resolution depends on instrument mode and may vary. For science purposes, using median values on a scale of 1-5 minutes is recommended.
- Halo to core electron temperature ratio from fits of selected QTN data [fit_t]
High resolution halo to core electron temperatures: resolution depends on instrument mode and may vary. For science purposes, using median values on a scale of 1-5 minutes is recommended.
- Halo to core electron temperature ratio uncertainty from fits of selected QTN data [delta_t]
High resolution halo to core electron temperatures: resolution depends on instrument mode and may vary. For science purposes, using median values on a scale of 1-5 minutes is recommended.
- Halo to core electron temperature ratio from fit initial guess [coarse_t]
High resolution halo to core electron temperatures: resolution depends on instrument mode and may vary. For science purposes, using median values on a scale of 1-5 minutes is recommended.
- Quality Flag of QTN fits of selected QTN data [QF]
Quality flags for fits of high resolution data: resolution depends on instrument mode and may vary. This variable is a weighted sum of other QF, calculated as QF = 5*QF_points + 3*QF_peak + QF_shift + QF_low_level, with maximum realistic value of 10. QF > 2 is considered good quality. QF > 5 is considered highly reliable.
- Quality Flag of QTN fits of selected QTN data; from number of selected QTN channels [QF_points]
Quality flags for fits of high resolution data: resolution depends on instrument mode and may vary. Normalized between 0 and 1.
- Quality Flag of QTN fits of selected QTN data; from fitting the plasma peak [QF_peak]
Quality flags for fits of high resolution data: resolution depends on instrument mode and may vary. Normalized between 0 and 1, although can rarely take values above 1.
- Quality Flag of QTN fits of selected QTN data; from shifts between fit and data [QF_shift]
Quality flags for fits of high resolution data: resolution depends on instrument mode and may vary. Normalized between 0 and 1.
- Quality Flag of QTN fits of selected QTN data; from data levels lower then the fit [QF_low_level]
Quality flags for fits of high resolution data: resolution depends on instrument mode and may vary. Normalized between 0 and 1.
- Filtered data for quick survey use (outliers labeled). [filtered]
Intervals seleceted for quick statistical survey usage (0 - filtered out; 1 - good for survey use). User is recomended to ignore the filter and use QFs for detailed examination of particular events.
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- WI_AT_DEF doi:10.48322/b88q-p434
- Description
TBS
- Modification History
6/13/91 - Original Implementation 9/18/91 - Modified for new attitude file format changes. ICCR 881 2/11/92 - Used the variable name TIME and type CDF_INT4 and size 3 instead of EPOCH, CDF_EPOCH and 1 for the time tags. CCR 490 6/1/92 - Added global attributes TITLE, PROJECT, DISCIPLINE, SOURCE_NAME, DATA_VERSION, and MODS; added variable attributes VALIDMIN, VALIDMAX, LABL_PTR_1, and MONOTON; added variables EPOCH and LABEL_TIME; changed variable name TIME to TIME_PB5. CCR 1066 11/07/92 - use cdf variable Epoch and Time_PB5 6/8/93 - Added global attributes ADID_ref and Logical_file_id. CCR 1092 7/5/94 - CCR ISTP 1852, updated CDHF skeleton to CDF standards - JT 9/20/94 - Added global attributes GCI_RA_ERR and GCI_DECL_ERR. CCR 1932 11/7/94 - Merged CCR 1852 changes and corrected errors made in CCR 1852. ICCR 1884 12/7/94 - Modified MODS and LABLAXIS to follow ISTP standards. ICCR 1885
- Data Variable Descriptions
- Body spin rate [BODY_SPIN_RATE]
- J2000 GCI right ascension [GCI_R_ASCENSION]
- J2000 GCI declination [GCI_DECLINATION]
- GSE right ascension [GSE_R_ASCENSION]
- GSE declination [GSE_DECLINATION]
- GSM right ascension [GSM_R_ASCENSION]
- GSM declination [GSM_DECLINATION]
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- WI_AT_PRE doi:10.48322/e07a-2494
- Description
TBS
- Modification History
6/13/91 - Original Implementation 9/18/91 - Modified for new attitude file format changes. ICCR 881 2/11/92 - Used the variable name TIME and type CDF_INT4 and size 3 instead of EPOCH, CDF_EPOCH and 1 for the time tags. CCR 490 6/1/92 - Added global attributes TITLE, PROJECT, DISCIPLINE, SOURCE_NAME, DATA_VERSION, and MODS; added variable attributes VALIDMIN, VALIDMAX, LABL_PTR_1, and MONOTON; added variables EPOCH and LABEL_TIME; changed variable name TIME to TIME_PB5. CCR 1066 11/07/92 - use cdf variable Epoch and Time_PB5 6/8/93 - Added global attributes ADID_ref and Logical_file_id. CCR 1092 7/5/94 - CCR ISTP 1852, updated CDHF skeleton to CDF standards - JT 9/20/94 - Added global attributes GCI_RA_ERR and GCI_DECL_ERR. CCR 1932 11/7/94 - Merged CCR 1852 changes and corrected errors made in CCR 1852. ICCR 1884 12/7/94 - Modified MODS and LABLAXIS to follow ISTP standards. ICCR 1885
- Data Variable Descriptions
- Body spin rate [BODY_SPIN_RATE]
- J2000 GCI right ascension [GCI_R_ASCENSION]
- J2000 GCI declination [GCI_DECLINATION]
- GSE right ascension [GSE_R_ASCENSION]
- GSE declination [GSE_DECLINATION]
- GSM right ascension [GSM_R_ASCENSION]
- GSM declination [GSM_DECLINATION]
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- WI_EHPD_3DP doi:10.48322/63fs-yr96
- Description
Wind 3dp, EESA High electron pitch angle distributions Note per Lynn Wilson Jan 2015 wrt time resolution: 24 sec timing changes and is not necessarily constant, depending on the mode that the instrument happens to be in. Not only does the period/interval between each point change, the duration over which the data were taken can change as well.
- Data Variable Descriptions
- Electron number flux 100eV-30keV in 15 energy and 8 angle bins (as energy-pitch angle displays) [FLUX]
- Electron number flux 100eV-30keV at 8 pitch angles as spectrograms by energy [FLUX_byE_atA]
- Electron number flux 100eV-30keV as a stack_plot of 15 energies at the Bin1 angle (often ~15 deg [FLUX_byE_atA_stackPA0]
- ---> As a stack_plot at the Bin2 angle (often ~35 deg) [FLUX_byE_atA_stackPA1]
- ---> As a stack_plot at the Bin3 angle (often ~57 deg) [FLUX_byE_atA_stackPA2]
- ---> As a stack_plot at the Bin4 angle (often ~80 deg) [FLUX_byE_atA_stackPA3]
- ---> As a stack_plot at the Bin5 angle (often ~102 deg) [FLUX_byE_atA_stackPA4]
- ---> As a stack_plot at the Bin6 angle (often ~123 deg) [FLUX_byE_atA_stackPA5]
- ---> As a stack_plot at the Bin7 angle (often ~145 deg) [FLUX_byE_atA_stackPA6]
- ---> As a stack_plot at the Bin8 angle (often ~165 deg) [FLUX_byE_atA_stackPA7]
- Electron number flux 100eV-30KeV at 8 select energies as spectrograms by pitch angle [FLUX_byA_atE]
- Electron number flux 100eV-30keV as a stack_plot of 8 pitch angles at the Ch1 energy (often ~28000 eV) [FLUX_byA_atE_stackE0]
- ---> As a stack plot at the Ch3 energy (often ~13000 eV) [FLUX_byA_atE_stackE2]
- ---> As a stack plot at the Ch5 energy (often ~6100 eV) [FLUX_byA_atE_stackE4]
- ---> As a stack plot at the Ch7 energy (often ~2900 eV) [FLUX_byA_atE_stackE6]
- ---> As a stack plot at the Ch9 energy (often ~1300eV) [FLUX_byA_atE_stackE8]
- ---> As a stack plot at the Ch11 energy (often ~630 eV) [FLUX_byA_atE_stackE10]
- ---> As a stack plot at the Ch13 energy (often ~300 eV) [FLUX_byA_atE_stackE12]
- ---> As a stack plot at the Ch15 energy (often ~140 eV) [FLUX_byA_atE_stackE14]
- Time-varying pitch angles for 8 angular bins [PANGLE]
- ---> Time-varying electron energies for 15 channels [ENERGY_filled]
Uses fix-sparse to fill in nan energy values
- SW Velocity vector (from ions and ground-based processing) [VSW]
- Vector magnetic field [MAGF]
- UNIX Time (secs since 1 Jan 1970) [TIME]
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- WI_EHSP_3DP doi:10.48322/c201-q577
- Description
Wind 3dp, EESA HIGH electron omni directional energy spectra Note per Lynn Wilson Jan 2015 wrt time resolution: 24 sec timing changes and is not necessarily constant, depending on the mode that the instrument happens to be in. Not only does the period/interval between each point change, the duration over which the data were taken can change as well.
- Data Variable Descriptions
- Electron differential number flux 100 eV - 30 keV, as a function of energy [spectrogram] [FLUX]
- ---> As stacked plot [FLUX_STACKED]
- ---> As time series [FLUX_SIMPLE]
- ---> Time-varying electron energies for 15 channels [ENERGY]
- UNIX Time (secs since 1 Jan 1970) [TIME]
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- WI_ELM2_3DP doi:10.48322/4tk0-a011
- Description
Wind 3dp, ELM2 Lynn Wilson Note Feb2015 Correct spacecraft potential is important to scientifically useful results .No documentation found on how this potential has been calculated.
- Data Variable Descriptions
- [SC_POT] Spacecraft potential estimated from electron ONLY measurements [SC_POT]
- ---> [SC_CURRENT?] Current contribution to the spacecraft from thermal electrons [SC_CURRENT]
- ---> [MAGF] magnetic field vector interpolated (linearly) to the time of the EESA Low distribution, in GSE cartesian components [MAGF]
- ---> [DENSITY] Electron number density [DENSITY]
- ---> [AVGTEMP] Average electron temperature [AVGTEMP]
- ---> [VTHERMAL] electron most probable speed [VTHERMAL]
- ---> [VELOCITY] electron Flow Velocity, GSE cartesian [VELOCITY]
- ---> [FLUX] electron total number flux - cartesian GSE [FLUX]
- [PTENS] electron Pressure Tensor calculated in the GSE coordinate basis. The elements correspond to, in the following order: XX, YY, ZZ, XY, XZ, YZ [PTENS]
- ---> [MFTENS] electron Momentum Flux Tensor calculated in the GSE coordinate basis. The elements correspond to, in the following order: XX, YY, ZZ, XY, XZ, YZ [MFTENS]
- ---> [EFLUX] eflux [EFLUX]
- ---> [T3] electron Temperature eigenvalues after diagonalization of tensor, calculated in the GSE coordinate basis. The elements correspond to: XX, YY, ZZ [T3]
- [SYMM] ZZ-component of the eigenvectors associated with the eigen values from the diagonalized .T3 (i.e., the eigenvector associated with the Z eigen value from .T3 or .T3[2]) [SYMM]
- ---> [SYMM_THETA] Spherical coordinate latitude of .SYMM [SYMM_THETA]
- ---> [SYMM_PHI] Spherical coordinate longitude of .SYMM [SYMM_PHI]
- ---> [SYMM_ANG] angle between the ZZ-component of the eigenvectors associated with the eigen values from the diagonalized .T3 and the magnetic field vector (i.e., .MAGF vector) [SYMM_ANG]
- ---> [MAGT3] electron temperature tensor... rotated into a field-aligned coordinate basis and then taking the diagonal elements only [MAGT3]
The elements then correspond to: Perp_1, Perp_2, Parallel (with respect to .MAGF). Let V = .VELOCITY, B = .MAGF, then: Perp_1 = (B x V) x B, Perp_2 = (B x V) and Then T_perp = (MAGT3[0] + MAGT3[1])/2.
- [P.ERANGE] electron energy range used to compute the moments [ERANGE]
- ---> [MASS] electron mass of species [MASS]
Units are eV/c^2, where c = speed of light in units of km/s. This results is a value of ~5.68566 x 10^(-6) for electrons and ~0.0104389 for protons.
- ---> [VALID] electron Validity flag; 1=OK [VALID]
- [VEL_MAG] electron bulk flow speed [VEL_MAG]
- ---> [VEL_TH] electron bulk flow velocity; latitude/theta [VEL_TH]
- ---> [VELPHI] electron bulk flow velocity; longitude/phi [VEL_PHI]
- UNIX time; seconds since January 1, 1970 [TIME]
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- WI_ELPD_3DP doi:10.48322/kesf-re26
- Description
Wind 3dp, EESA Low electron pitch angle distributions with ion-derived moments
- Data Variable Descriptions
- Electron number flux 5-1100 eV in 15 energy and 8 angle bins (as energy-pitch angle displays) [FLUX]
- Electron number flux 5-1100 eV at 8 pitch angles as spectrograms by energy [FLUX_byE_atA]
- Electron number flux 5-1100 eV as a stack_plot of 15 energies at the Bin1 angle (often ~15 deg [FLUX_byE_atA_stackPA0]
- ---> As a stack_plot at the Bin2 angle (often ~35 deg) [FLUX_byE_atA_stackPA1]
- ---> As a stack_plot at the Bin3 angle (often ~57 deg) [FLUX_byE_atA_stackPA2]
- ---> As a stack_plot at the Bin4 angle (often ~80 deg) [FLUX_byE_atA_stackPA3]
- ---> As a stack_plot at the Bin5 angle (often ~102 deg) [FLUX_byE_atA_stackPA4]
- ---> As a stack_plot at the Bin6 angle (often ~123 deg) [FLUX_byE_atA_stackPA5]
- ---> As a stack_plot at the Bin7 angle (often ~145 deg) [FLUX_byE_atA_stackPA6]
- ---> As a stack_plot at the Bin8 angle (often ~165 deg) [FLUX_byE_atA_stackPA7]
- Electron number flux 5-1100 eV at 8 select energies as spectrograms by pitch angle [FLUX_byA_atE]
- Electron number flux 5-1100 eV as a stack_plot of 8 pitch angles at the Ch1 energy (often ~1150 eV) [FLUX_byA_atE_stackE0]
- ---> As a stack plot at the Ch3 energy (often ~540 eV) [FLUX_byA_atE_stackE2]
- ---> As a stack plot at the Ch5 energy (often ~255 eV) [FLUX_byA_atE_stackE4]
- ---> As a stack plot at the Ch7 energy (often ~121 eV) [FLUX_byA_atE_stackE6]
- ---> As a stack plot at the Ch9 energy (often ~58 eV) [FLUX_byA_atE_stackE8]
- ---> As a stack plot at the Ch11 energy (often ~29 eV) [FLUX_byA_atE_stackE10]
- ---> As a stack plot at the Ch13 energy (often ~15 eV) [FLUX_byA_atE_stackE12]
- ---> As a stack plot at the Ch15 energy (often ~8.6 eV) [FLUX_byA_atE_stackE14]
- Time-varying pitch angles for 8 angular bins [PANGLE]
- ---> Time-varying electron energies for 15 channels [ENERGY]
- SW Velocity vector (from ions and ground-based processing) [VSW]
- Vector magnetic field [MAGF]
- UNIX Time (secs since 1 Jan 1970) [TIME]
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- WI_ELSP_3DP doi:10.48322/cbvx-4034
- Description
Wind 3dp, EESA Low omni directional electron energy spectra
- Data Variable Descriptions
- Electron differential number flux as function of time-varying energy in range 5-1100 eV [as spectrogram] [FLUX]
- ---> As stacked plot [FLUX_STACKED]
- ---> As simple time series [FLUX_SIMPLE]
- Time-varying electron energies in 15 channels (center of 40% wide energy band) [ENERGY]
- UNIX time; seconds since January 1, 1970 [TIME]
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- WI_EMFITS_E0_3DP doi:10.48322/ndp9-8t38
- Description
These electron parameters are moments of Wind 3DP EESA-L and EESA-H measurements, corrected for spacecraft potential and other instrumental effects. More information can be found at: R. P. Lin et al., A Three-dimensional plasma and energetic particle investigation for the Wind spacecraft, Space Science Reviews, Vol. 71, p125-153, 1995. C. S. Salem et al., Precision Electron Measurements in the Solar Wind at 1AU from NASA’s Wind spacecraft, J. Geophys. Res. Space Physics, 2017. M. Pulupa et al., Spin-modulated spacecraft floating potential: Observations and effects on electron moments, J. Geophys. Res. Space Physics, Vol. 119, 647-657, doi:10.1002/2013JA019359, 2014.
- Data Variable Descriptions
- Total electron density moment in units of /cm^3 [N_e_dens_wi_3dp]
Total electron density moment from EESA-L and EESA-H
- Parallel total electron temperature moment in units of eV [T_e_par_wi_3dp]
Includes EESA-L and EESA-H data
- Perpendicular total electron temperature moment in units of eV [T_e_perp_wi_3dp]
Includes EESA-L and EESA-H data
- Parallel electron heat flux moment in units of uW/m^2 [Q_e_par_wi_3dp]
Includes EESA-L and EESA-H data
- Electron velocity vector moment in GSE coordinates in units of km/s [V_e_xyz_gse_wi_3dp]
Includes EESA-L and EESA-H data
- Q0, Quality parameter for electron data [Quality0_wi_3dp]
Q0 is a quality parameter calculated from the properties of the input data and goodness-of-fit statistics from the nonlinear fitting process. It varies between 0 and 10. Higher values of Q0 represent more confidence in the resulting electron parameters
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- WI_EM_3DP doi:10.48322/bsy7-7789
- Description
Wind 3dp, EESA LOW 1 spin resolution Plasma ( electron ) moments (computed on spacecraft)
- Modification History
Version 3 Product, August 2005
- Data Variable Descriptions
- Electron number density (not corrected for any s/c potential) [E_DENS]
Per Lynn Wilson Jan2015: These results cannot take the spacecraft potential into account. Wind does not measure the spacecraft potential actively, so it cannot perform this correction onboard and the results have many uncertainties.
- ---> Electron velocity vector (GSE) [E_VELS]
- ---> Residual Variance in Electron Velocity (6 components in instrument coords) [E_TENS]
Per Lynn Wilson Jan2015: This is in one of two units. It is calculated as the pressure tensor divided by the number density. In the decommutation source code, they say the units are (km/s)^2. In some of the other moment analysis software, the pressure is in units of [eV cm^(-3)].
- ---> Electron temperature [E_TEMP]
- ---> Electron Heat Flux (Q) [E_Q]
Per Lynn Wilson Jan2015: This is the vector form of the electron heat flux. It should have units of either [(km/s)^3 cm^(-3)] or [eV km/s cm^(-3)] . I am guessing the former due to the .VV units used above, since this is usually given the structure tag .NVVV.
- Gap flag (0=no gap, 1=gap) [GAP]
- Data quality flag (1=good, 0=bad) [VALID]
- Unix Time (since 1970/01/01) [TIME]
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WI_EPACT_STEP-DIFFERENTIAL-ION-FLUX-1HR doi:10.48322/6654-mc20
Proper citations should include the "Accessed on date" in the form . - Description
The EPACT Instrument on Wind STEP - SupraThermal Energetic Particle Telescope measures ion fluxes of protons (H) in 0.12.5 MeV energy range and He-Fe nuclei in the ~0.032 MeV/nucleon energy ranges in two identical telescopes, each with a geometrical factor of 0.4 cm2 sr and a rectangular field
- Data Variable Descriptions
- H energy min [H_energy_min]
- H energy center [H_energy_center]
- H energy max [H_energy_max]
- H efficiency low [H_energy_efficiency_low]
- H efficieny high [H_energy_efficiency_high]
- H energy efficieny avg [H_energy_efficiency_avg]
- H energy center telescope 1 [H_ENERGY_CENTER_T1]
- H energy center telescope 2 [H_ENERGY_CENTER_T2]
- H flux [H_flux]
- H flux sigma [H_flux_sigma]
- H flux Telescope 1 [H_FLUX_T1]
- H flux Telescope 2 [H_FLUX_T2]
- He energy min [He_energy_min]
- He energy center [He_energy_center]
- He energy max [He_energy_max]
- He efficiency low [He_energy_efficiency_low]
- He efficieny high [He_energy_efficiency_high]
- He energy efficieny avg [He_energy_efficiency_avg]
- He energy center telescope 1 [HE_ENERGY_CENTER_T1]
- He energy center telescope 2 [HE_ENERGY_CENTER_T2]
- He flux [He_flux]
- He flux sigma [He_flux_sigma]
- He flux Telescope 1 [HE_FLUX_T1]
- He flux Telescope 2 [HE_FLUX_T2]
- CNO energy min [CNO_energy_min]
- CNO energy center [CNO_energy_center]
- CNO energy max [CNO_energy_max]
- CNO efficiency low [CNO_energy_efficiency_low]
- CNO efficieny high [CNO_energy_efficiency_high]
- CNO energy efficieny avg [CNO_energy_efficiency_avg]
- CNO energy center telescope 1 [CNO_ENERGY_CENTER_T1]
- CNO energy center telescope 2 [CNO_ENERGY_CENTER_T2]
- CNO flux [CNO_flux]
- CNO flux sigma [CNO_flux_sigma]
- CNO flux Telescope 1 [CNO_FLUX_T1]
- CNO flux Telescope 2 [CNO_FLUX_T2]
- NeS energy min [NeS_energy_min]
- NeS energy center [NeS_energy_center]
- NeS energy max [NeS_energy_max]
- NeS efficiency low [NeS_energy_efficiency_low]
- NeS efficieny high [NeS_energy_efficiency_high]
- NeS energy efficieny avg [NeS_energy_efficiency_avg]
- NeS energy center telescope 1 [NES_ENERGY_CENTER_T1]
- NeS energy center telescope 2 [NES_ENERGY_CENTER_T2]
- NeS flux [NeS_flux]
- NeS flux sigma [NeS_flux_sigma]
- NeS flux Telescope 1 [NES_FLUX_T1]
- NeS flux Telescope 2 [NES_FLUX_T2]
- Fe energy min [Fe_energy_min]
- Fe energy center [Fe_energy_center]
- Fe energy max [Fe_energy_max]
- Fe efficiency low [Fe_energy_efficiency_low]
- Fe efficieny high [Fe_energy_efficiency_high]
- Fe energy efficieny avg [Fe_energy_efficiency_avg]
- Fe energy center telescope 1 [FE_ENERGY_CENTER_T1]
- Fe energy center telescope 2 [FE_ENERGY_CENTER_T2]
- Fe flux [Fe_flux]
- Fe flux sigma [Fe_flux_sigma]
- Fe flux Telescope 1 [FE_FLUX_T1]
- Fe flux Telescope 2 [FE_FLUX_T2]
- B [B]
- Btheta [Btheta]
- Bphi [Bphi]
- Brms [Brms]
- R [R]
- xyz gse [xyzGSE]
- Vsw [Vsw]
- velocity [velocity]
- Np [Np]
- Vth [Vth]
- spin_rate [spin_rate]
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WI_EPACT_STEP-DIRECTIONAL-DIFF-CNO-FLUX-10MIN doi:10.48322/0y67-vc97
Proper citations should include the "Accessed on date" in the form . - Description
The EPACT Instrument on Wind STEP - SupraThermal Energetic Particle Telescope measures ion fluxes of protons (H) in 0.12.5 MeV energy range and He-Fe nuclei in the ~0.032 MeV/nucleon energy ranges in two identical telescopes, each with a geometrical factor of 0.4 cm2 sr and a rectangular field of view with an angular acceptance of 44 deg in azimuth and 17 deg in polar angle.
- Data Variable Descriptions
- CNO energy center telescope 1 [ENERGY_CENTER_T1]
- CNO energy center telescope 2 [ENERGY_CENTER_T2]
- CNO flux Telescope 1 (as energy-pitch angle displays) [FLUX_T1]
- CNO flux Telescope 2 (as energy-pitch angle displays) [FLUX_T2]
- CNO flux for telescope 1 at 8 pitch angles as spectrograms by energy [flux_t1_byE_atA]
- CNO flux for telescope 2 at 8 pitch angles as spectrograms by energy [flux_t2_byE_atA]
- CNO flux for telescope 1 at 7 energies as spectrograms by pitch angle [flux_t1_byA_atE]
- CNO flux for telescope 2 at 7 energies as spectrograms by pitch angle [flux_t2_byA_atE]
- B [B]
- Btheta [Btheta]
- Bphi [Bphi]
- Brms [Brms]
- R [R]
- xyz gse telescope 1 [xyzGSE_T1]
- xyz gse telescope 2 [xyzGSE_T2]
- Vsw [Vsw]
- velocity telescope 1 [velocity_T1]
- velocity telescope 2 [velocity_T2]
- Np [Np]
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WI_EPACT_STEP-DIRECTIONAL-DIFF-FE-FLUX-10MIN doi:10.48322/t2mh-c690
Proper citations should include the "Accessed on date" in the form . - Description
The EPACT Instrument on Wind STEP - SupraThermal Energetic Particle Telescope measures ion fluxes of protons (H) in 0.12.5 MeV energy range and He-Fe nuclei in the ~0.032 MeV/nucleon energy ranges in two identical telescopes, each with a geometrical factor of 0.4 cm2 sr and a rectangular field of view with an angular acceptance of 44 deg in azimuth and 17 deg in polar angle.
- Data Variable Descriptions
- FE energy center telescope 1 [ENERGY_CENTER_T1]
- FE energy center telescope 2 [ENERGY_CENTER_T2]
- FE flux Telescope 1 (as energy-pitch angle displays) [FLUX_T1]
- FE flux Telescope 2 (as energy-pitch angle displays) [FLUX_T2]
- FE flux for telescope 1 at 8 pitch angles as spectrograms by energy [flux_t1_byE_atA]
- FE flux for telescope 2 at 8 pitch angles as spectrograms by energy [flux_t2_byE_atA]
- FE flux for telescope 1 at 6 energies as spectrograms by pitch angle [flux_t1_byA_atE]
- FE flux for telescope 2 at 6 energies as spectrograms by pitch angle [flux_t2_byA_atE]
- B [B]
- Btheta [Btheta]
- Bphi [Bphi]
- Brms [Brms]
- R [R]
- xyz gse telescope 1 [xyzGSE_T1]
- xyz gse telescope 2 [xyzGSE_T2]
- Vsw [Vsw]
- velocity telescope 1 [velocity_T1]
- velocity telescope 2 [velocity_T2]
- Np [Np]
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WI_EPACT_STEP-DIRECTIONAL-DIFF-H-FLUX-10MIN doi:10.48322/c7fp-nf79
Proper citations should include the "Accessed on date" in the form . - Description
The EPACT Instrument on Wind STEP - SupraThermal Energetic Particle Telescope measures ion fluxes of protons (H) in 0.12.5 MeV energy range and He-Fe nuclei in the ~0.032 MeV/nucleon energy ranges in two identical telescopes, each with a geometrical factor of 0.4 cm2 sr and a rectangular field of view with an angular acceptance of 44 deg in azimuth and 17 deg in polar angle.
- Data Variable Descriptions
- H flux for telescope 1 at 8 pitch angles as spectrograms by energy [flux_t1_byE_atA]
- H flux for telescope 2 at 8 pitch angles as spectrograms by energy [flux_t2_byE_atA]
- H flux for telescope 1 at 10 energies as spectrograms by pitch angle [flux_t1_byA_atE]
- H flux for telescope 2 at 10 energies as spectrograms by pitch angle [flux_t2_byA_atE]
- H flux Telescope 1 (as energy-pitch angle displays) [FLUX_T1]
- H flux Telescope 2 (as energy-pitch angle displays) [FLUX_T2]
- H energy center telescope 1 [ENERGY_CENTER_T1]
- H energy center telescope 2 [ENERGY_CENTER_T2]
- B [B]
- Btheta [Btheta]
- Bphi [Bphi]
- Brms [Brms]
- R [R]
- xyz gse telescope 1 [xyzGSE_T1]
- xyz gse telescope 2 [xyzGSE_T2]
- Vsw [Vsw]
- velocity telescope 1 [velocity_T1]
- velocity telescope 2 [velocity_T2]
- Np [Np]
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WI_EPACT_STEP-DIRECTIONAL-DIFF-HE-FLUX-10MIN doi:10.48322/z4p2-ky35
Proper citations should include the "Accessed on date" in the form . - Description
The EPACT Instrument on Wind STEP - SupraThermal Energetic Particle Telescope measures ion fluxes of protons (H) in 0.12.5 MeV energy range and He-Fe nuclei in the ~0.032 MeV/nucleon energy ranges in two identical telescopes, each with a geometrical factor of 0.4 cm2 sr and a rectangular field of view with an angular acceptance of 44 deg in azimuth and 17 deg in polar angle.
- Data Variable Descriptions
- HE energy center telescope 1 [ENERGY_CENTER_T1]
- HE energy center telescope 2 [ENERGY_CENTER_T2]
- HE flux Telescope 1 (as energy-pitch angle displays) [FLUX_T1]
- HE flux Telescope 2 (as energy-pitch angle displays) [FLUX_T2]
- HE flux for telescope 1 at 8 pitch angles as spectrograms by energy [flux_t1_byE_atA]
- HE flux for telescope 2 at 8 pitch angles as spectrograms by energy [flux_t2_byE_atA]
- HE flux for telescope 1 at 7 energies as spectrograms by pitch angle [flux_t1_byA_atE]
- HE flux for telescope 2 at 7 energies as spectrograms by pitch angle [flux_t2_byA_atE]
- B [B]
- Btheta [Btheta]
- Bphi [Bphi]
- Brms [Brms]
- R [R]
- xyz gse telescope 1 [xyzGSE_T1]
- xyz gse telescope 2 [xyzGSE_T2]
- Vsw [Vsw]
- velocity telescope 1 [velocity_T1]
- velocity telescope 2 [velocity_T2]
- Np [Np]
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- WI_H0_MFI doi:10.48322/av38-wn55
- Description
WIND MFI Composite data file. This file contains multiple time resolution data. 1 Minute data averages 3 Second data averages 1 Hour data averages WIND MFI Instrument turn on 11/12/1994 Data versions: 03 - Extrapolated Bz correction 04 - Final Bz correction 05 - Final orbit and Bz correction References: 1. Lepping, R. P., et al., The WIND Magnetic Field Investigation, p. 207 in The Global Geospace Mission, ed. by C. T. Russell, Kluwer,1995 2. Panetta, P. (GSFC), GGS WIND MFI Operator's Manual, September 15, 1992. 3. Computer Sciences Corporation, Data Format Control Document (DFCD) Between The International Solar-Terrestrial Physics (ISTP) Program Information Processing Division Ground Data Processing System and The ISTP Mission Investigators, CSC/TR-91/6014, 560-1DFD/0190, July 1992. 4. Behannon, K. W., International Solar Terrestrial Physics (ISTP) Program Investigator Data Analysis Requirements For WIND and GEOTAIL Spacecraft Magnetometer Experiment, September 1987. 5. National Space Science Data Center, CDF User's Guide, Version 2.3.0, October 1, 1992. 6. Mish, W. H., International Solar-Terrestrial Physics (ISTP) Key Parameter Generation Software (KPGS) Standards & Conventions, September 1992. 7. Mish, W. H., IMP F and G Phase I Magnetic Field Analysis, April 1972
- Modification History
10/01/2011 Initial release
- Data Variable Descriptions
- Magnetic field magnitude (1 min) [BF1]
Average of the magnitudes (F1)
- Magnetic field magnitude (1 min - log scaled) [BF1LOG]
Average of the magnitudes (F1)
- RMS magnitude (1 min) [BRMSF1]
RMS of the magnitudes (F1 RMS)
- Magnetic field vector in GSM cartesian coordinates (1 min) [BGSM]
- RMS vector in GSM coordinates (1 min) [BRMSGSM]
- Magnetic field vector in GSE cartesian coordinates (1 min) [BGSE]
- Magnetic field vector in GSE angular coordinates (1 min) [BGSEa]
- RMS vector in GSE coordinates (1 min) [BRMSGSE]
- Distance from the center of the earth (Define Re = 6378km) (1 min) [DIST]
- Position vector in GSM coordinates (Define Re = 6378km) (1 min) [PGSM]
- Position vector in GSE coordinates (Define Re = 6378km) (1 min) [PGSE]
- Magnetic field magnitude (3 sec) [B3F1]
Average of the magnitudes (F1)
- Magnetic field magnitude (3 sec - log scaled) [B3F1LOG]
Average of the magnitudes (F1)
- RMS magnitude (3 sec) [B3RMSF1]
RMS of the magnitudes (F1 RMS)
- Magnetic field vector in GSM cartesian coordinates (3 sec) [B3GSM]
- RMS vector in GSM coordinates (3 sec) [B3RMSGSM]
- Magnetic field vector in GSE cartesian coordinates (3 sec) [B3GSE]
- Magnetic field vector in GSE angular coordinates (3 sec) [B3GSEa]
- RMS vector in GSE coordinates (3 sec) [B3RMSGSE]
- Magnetic field magnitude (1 hour) [B1F1]
Average of the magnitudes (F1)
- Magnetic field magnitude (1 hour - log scaled) [B1F1LOG]
Average of the magnitudes (F1)
- RMS magnitude (1 hour) [B1RMSF1]
RMS of the magnitudes (F1 RMS)
- Magnetic field vector in GSM cartesian coordinates (1 hour) [B1GSM]
- RMS vector in GSM coordinates (1 hour) [B1RMSGSM]
- Magnetic field vector in GSE cartesian coordinates (1 hour) [B1GSE]
- Magnetic field vector in GSE angular coordinates (1 hour) [B1GSEa]
- RMS vector in GSE coordinates (1 hour) [B1RMSGSE]
- Distance from the center of the earth (Define Re = 6378km) (1 hour) [DIST1]
- Position vector in GSM coordinates (Define Re = 6378km) (1 hour) [P1GSM]
- Position vector in GSE coordinates (Define Re = 6378km) (1 hour) [P1GSE]
- Time axis label: Distance from the center of the earth (Define Re = 6378km) (1 min) [DISTV]
- Time axis label: Position vector in GSM coordinates (Define Re = 6378km) (1 min) [PGSMV]
- Time axis label: Position vector in GSE coordinates (Define Re = 6378km) (1 min) [PGSEV]
- Time axis label: Distance from the center of the earth (Define Re = 6378km) (1 hour) [DIST1V]
- Time axis label: Position vector in GSM coordinates (Define Re = 6378km) (1 hour) [P1GSMV]
- Time axis label: Position vector in GSE coordinates (Define Re = 6378km) (1 hour) [P1GSEV]
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- WI_H0_SWE doi:10.48322/2jxp-7x36
- Description
Explanatory notes: The electron moments included in this data set are derived from the velocity moments integration of solar wind electron distributions measured by the WIND/SWE VEIS instrument (see Ogilvie et al., "SWE, a comprehensive plasma instrument for the WIND spacecraft", Space Sci. Rev., 71, 55, 1955). Moments parameters are computed from 3s measurements which are spaced either 6s or 12s in time. Plots should therefore not exceed a time range of 2 or 3 hours in order to display the details of this high resolution data. The moments parameters which will be of value to most users of this data set are the electron temperature, the electron temperature anisotropy, and the electron heat flux vector. These quantities are reliable and citable with caution, meaning that the PI advises that the user should discuss their interpretation with a member of the SWE science team before publishing. The following comments are intended to aid in the use and interpretation of the prime quantities of this data set, the electron temperature, the electron temperature anisotropy, and the electron heat flux. (All vector quantities are in GSE coordinates.) The temperature and temperature anisotropy are normalized to the derived electron density and, therefore, are not sensitive to the uncertainty in the density determination as discussed below. The electron temperature is derived from the pressure tensor divided by the electron density and the Boltzmann constant. The three eigenvalues of the diagonalized temperature tensor are the temperature parallel to the tensor principal axis and the two perpendicular components of the temperature. The temperature anisotropy is defined here as the ratio of the parallel temperature to the average of the two perpendicular temperature components. The electron temperature is one-third of the trace of the diagonalized temperature tensor. Also included is the unit vector along the principal axis of the pressure tensor as well as the cosine of the angle between the principal axis and the magnetic field vector. An indication that the principal axis has been uniquely defined is that the temperature anisotropy is significantly different from unity and that the principal axis and the magnetic field are nearly parallel or anti-parallel. The heat flux vector included here is significant only when the magnitude rises above the noise level, i.e., above the level 0.002 to 0.005 ergs/cm/cm/s. The heat flux may be low in magnitude either due to a nearly isotropic distribution, due to electron counter-streaming, or due to a low counting rate of the instrument. An indicator of a significant net heat flux is that the heat flux direction should track with the magnetic field direction. For this purpose, the cosine of the angle between the heat flux vector and the magnetic field is included, and should be close to -1 or +1 in order for the heat flux to be significant. In some cases it will be necessary to use electron pitch angle distributions (available on request from the SWE team) to decide whether low electron flux or counterstreaming account for a low net heat flux. It is also strongly recommended that 3s magnetic field data from the WIND/MFI experiment (not included in this data set) be used in conjunction with the SWE electron heat flux data to ensure a correct interpretation of the heat flux. The electron density and electron bulk flow velocity are also included in this data set but no claim is made for their accuracy. The electron flow velocity is usually within 10% to 20% of the solar wind flow velocity derived from the SWE Faraday cup experiment and which are found in the SWE key parameter data set. The electron density, however, cannot be absolutely determined due to the spacecraft potential and the fact that the electron instrument response has varied over time. The electron density determination includes a first order attempt to determine the spacecraft potential by imposing the charge neutrality condition on the derived electron density and Faraday cup ion density. The electron density will be within a few percent of the solar wind density derived from the Faraday cup early in the mission (1994-1997), while later in the mission (1998 and onward), depending on the state of the instrument, there will be times when the derived electron density may be as much as a factor 2 too low. Although the electron density is not derived absolutely, relative changes in electron density can usually be relied on. Both the electron density and electron flow speed track with variations in the ion density and ion flow speed, respectively. However, the user is strongly advised to use the SWE ion key parameters for the bulk plasma density and flow speed.
- Modification History
Skeleton created 1/19/2000 Started again 3/13/2001
- Data Variable Descriptions
- Electron Temperature, Te [Te]
Te = (trace of pressure tensor)/(electron density * Boltzman constant)/3 = (2*Te_perp + Te_para)/3
- Temperature anisotropy = Te_para / Te_perp [Te_anisotropy]
Te_perp = average of the perpendicular elements of the temperature tensor. Te_para = parallel component of the temperature tensor.
- Electron average energy [average_energy]
Average energy = (3/2)Boltzmann constant * Te
- Principle axis of pressure tensor - unit vector [pa_press_tensor]
- Pressure tensor principle axis dot magnetic field unit vector [pa_dot_B]
- Electron heat flux magnitude [heat_flux_magn]
- Electron heat flux elevation [heat_flux_el]
- Electron heat flux azimuth [heat_flux_az]
- Heat flux dot B unit vector [Q_dot_B]
- Spacecraft Position (GSE) [sc_position]
- Electron bulk velocity - magnitude [el_bulk_vel_magn]
See the global attribute TEXT.
- Electron bulk velocity - elevation [el_bulk_vel_el]
See the global attribute TEXT.
- Electron bulk velocity - azimuth [el_bulk_vel_az]
See the global attribute TEXT.
- Electron density [el_density]
See the global attribute TEXT.
- Spacecraft Potential [sc_pot]
Forst-order estimate only; se the global attribute TEXT.
- Quality Flag, yet to be defined [flag]
- major frame record number [major_fr_rec]
- Major frame spin number [major_fr_spin_number]
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- WI_H0_WAV doi:10.48322/thkc-wf80
- Description
SSR WAVES: The Radio and Plasma Wave Investigation on the WIND Spacecraft, Vol 71, pg 231-263,1995. Secondary file - high resplasma density
- Modification History
CODED JUNE 1996, C. MEETRE
- Data Variable Descriptions
- Electron density determined from insitu Fpe 'line' position recognized by a neural network. [Ne]
High resolution plasma densities: actual resolution depends on instrument mode and may vary.
- Electric field power in dB at the peak frequency selected by the neural network algorithm [Ne_peak]
No background subtraction - spin plane
- Electron Density data quality: <50=bad,>50=Fair,>150=ok,>200=good [Ne_Quality]
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- WI_H1_SWE doi:10.48322/nasd-j276
- Description
SWE, a comprehensive plasma instrument for the WIND spacecraft, K.W. Ogilvie, et al., Space Sci. Rev., 71, 55-77, 1995 Solar wind proton parameters, including anisotropic temperatures, derived by non-linear fitting of the measurements and with moment techniques. Data reported within this file do not exceed the limits of various parameters listed in the following section. There may be more valid data in the original dataset that requires additional work to interpret but was discarded due to the limits. In particular we have tried to exclude non-solar wind data from these files. We provide the one sigma uncertainty for each parameter produced by the non-linear curve fitting analysis either directly from the fitting or by propagating uncertainties for bulk speeds, flow angles or any other derived parameter. For the non-linear anisotropic proton analysis, a scalar thermal speed is produced by determining parallel and perpendicular temperatures, taking the trace, Tscalar = (2Tperp + Tpara)/3 and converting the result back to a thermal speed. The uncertainties are also propagated through Notes: Data reported within this file do not exceed the limits of various paremeters listed in the following section. There may be more valid data in the original dataset that require additional work to interpret but was discarded due to the limits. In particular we have tried to exclude non-solar wind data and questionable alpha data from these files. We provide the one sigma uncertainty for each parameter produced by the non-linear curve fitting analysis either directly from the fitting or by propagating uncertainties for bulk speeds, flow angles or any other derived parameter. For the non-linear anisotropic proton analysis, a scalar thermal speed is produced by determining parallel and perpendicular tmperatures, taking the trace, Tscalar = (2Tperp + Tpara)/3 and converting the result back to a thermal speed. The uncertainties are also. propagated through Limits: Minimum mach number: 1.5000000; Maximum chisq/dof: 100000.00; Minimum distance; to bow shock: 5.0000000 [Re]; Maximum uncertainty in any; parameter from non-linear;analysis: 70.0000[%]. - Modification History
data analysis package revised March, 2012.
- Data Variable Descriptions
- This flag denotes the fit quality and encodes any contingencies in the ion VDF analysis (10=SW parameters OK) [fit_flag]
FLAG values indicate analysis contingencies:. .10: Solar wind parameters OK -- no action necessary..9: Alpha particles relatively too cold..8: Alpha particles overlap within protons in CDF. ..7: Alphas too fast, out of SWE range..6: Alpha particle peak may be confused with second proton peak...5: Parameters OK, but Tp=Ta constraint used (params obtained with SUB_PROT=1) ..4: alphas are unusually cold, Tp=Ta constraint used (SUB_PROT=1)..3: alpha patr. relatively too hot (SUB_PROT=1). Tp=Ta constraint used..2: The speed of the alpha is unusually low. ..1: Poor peak identification..0: Spectrum cannot be fit with a bimax model..
- ---> year [year]
- ---> Fractional day of year of start of spectrum (Noon on January 1 = 1.5) [doy]
- Proton bulk speed [Proton_V_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> Proton bulk speed (w/ uncertainties) [Proton_V_nonlin_errorbars]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> 1-sigma uncertainty of the proton bulk speed [Proton_sigmaV_nonlin]
From fit uncertainty, measurement uncertainties
- VX_GSE component of the proton vector velocity [km/s], from non-linear analysis [Proton_VX_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> VX_GSE (with uncertainties) [Proton_VX_nonlin_errorbars]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> 1-sigma uncertainty of VX_GSE [Proton_sigmaVX_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- VY_GSE component of the proton vector velocity [km/s], from non-linear analysis [Proton_VY_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> VY_GSE (with uncertainties) [Proton_VY_nonlin_errorbars]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> 1-sigma uncertainty of VY_GSE [Proton_sigmaVY_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- VZ_GSE component of the proton vector velocity [km/s], from non-linear analysis [Proton_VZ_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> VZ_GSE (with uncertainties) [Proton_VZ_nonlin_errorbars]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> 1-sigma uncertainty of VZ_GSE [Proton_sigmaVZ_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- Scalar [isotropic] proton thermal speed [km/s], from the trace of the anisotropic temperatures. [Proton_W_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> Scalar [isotropic] proton thermal speed (with uncertainties) [Proton_W_nonlin_errorbars]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> 1-sigma uncertainty in the proton thermal speed [km/s]. [Proton_sigmaW_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- Proton thermal speed perpendicular to the magnetic field direction [km/s]. [Proton_Wperp_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> Proton thermal speed perpendicular (with uncertainties) [Proton_Wperp_nonlin_errorbars]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> 1-sigma uncertainty in the perpendicular proton thermal speed [km/s]. [Proton_sigmaWperp_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- Proton thermal speed parallel to the magnetic field direction [km/s]. [Proton_Wpar_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> Proton thermal speed parallel (with uncertainties) [Proton_Wpar_nonlin_errorbars]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> 1-sigma uncertainty in the parallel proton thermal speed [km/s]. [Proton_sigmaWpar_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- East-West GSE bulk Flow Angle [degrees] [EW_flowangle]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> East-West Flow Angle (with uncertainties) [EW_flowangle_errorbars]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> 1-sigma uncertainty in the east-west flow angle [SigmaEW_flowangle]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- North-south GSE bulk flow angle [degrees] [NS_flowangle]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> North-south flow angle (with uncertainties) [NS_flowangle_errorbars]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> 1-sigma uncertainty in north-south flow angle [SigmaNS_flowangle]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- Proton number density Np (n/cc) from non-linear analysis [Proton_Np_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> Proton number density Np (log scale) [Proton_Np_nonlin_log]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> Proton number density Np (with uncertainties) [Proton_Np_nonlin_errorbars]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> 1-sigma uncertainty in the proton density [Proton_sigmaNp_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- Alpha bulk speed V (km/s) from non-linear analysis [Alpha_V_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> Alpha bulk speed V (with uncertainties) [Alpha_V_nonlin_errorbars]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> 1-sigma uncertainty in alpha V [km/s] [Alpha_sigmaV_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- Alpha velocity component Vx (GSE, km/s) from non-linear analysis [Alpha_VX_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> Alpha velocity component Vx (with uncertainties) [Alpha_VX_nonlin_errorbars]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> 1-sigma uncertainty in alpha Vx [km/s] [Alpha_sigmaVX_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- Alpha velocity component Vy (GSE, km/s) from non-linear analysis [Alpha_VY_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> Alpha velocity component Vy (with uncertainties) [Alpha_VY_nonlin_errorbars]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- --->1-sigma uncertainty in alpha Vy [km/s] [Alpha_sigmaVY_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- Alpha velocity component Vz (GSE, km/s) from non-linear analysis [Alpha_VZ_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> Alpha velocity component Vz (with uncertainties) [Alpha_VZ_nonlin_errorbars]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- --->1-sigma uncertainty in alpha Vz [km/s] [Alpha_sigmaVZ_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- Scalar [isotropic] alpha particle thermal speed [km/s]. [Alpha_W_nonlin]
Calculated from the trace of the anisotropic alpha pressure tensor, obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> Scalar [isotropic] alpha particle thermal speed [km/s] (with uncertainties) [Alpha_W_nonlin_errorbars]
Calculated from the trace of the anisotropic alpha pressure tensor, obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> 1-sigma uncertainty in alpha thermal speed [km/s]. [Alpha_sigmaW_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- Alpha particle thermal speed perpendicular to the magnetic field direction [km/s]. [Alpha_Wperp_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> Alpha particle thermal speed perpendicular (with uncertainties) [Alpha_Wperp_nonlin_errorbars]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> 1-sigma uncertainty in the perpendicular alpha thermal speed [km/s]. [Alpha_sigmaWperp_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- Alpha particle thermal speed parallel to the magnetic field direction [km/s] [Alpha_Wpar_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> Alpha particle thermal speed parallel (with uncertainties) [Alpha_Wpar_nonlin_errorbars]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> 1-sigma uncertainty in the perpendicular alpha thermal speed [km/s]. [Alpha_sigmaWpar_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- Alpha number density Na (n/cc) from non-linear analysis [Alpha_Na_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> Alpha number density Na (log scale) [Alpha_Na_nonlin_log]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> Alpha number density Na (with uncertainties) [Alpha_Na_nonlin_errorbars]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> 1-sigma uncertainty in the alpha density [n/cc] [Alpha_sigmaNa_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- Reduced chi-squared for this fit [ChisQ_DOF_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> Time that the peak charge flux was observed for each spectrum (in fractional day of year) [Peak_doy]
Statistical moments of the ion velocity distribution function (VDF) are estimated analytically from the ion current distribution function (CDF).
- ---> 1-sigma uncertainty in time of peak flux (in fractional day of year) [sigmaPeak_doy]
calculated from the number of spacecraft spins corresponding to the half-width measurement
- Proton bulk speed (km/s) from moment analysis [Proton_V_moment]
Statistical moments of the ion velocity distribution function (VDF) are estimated analytically from the ion current distribution function (CDF).
- Proton velocity component Vx (GSE, km/s) from moment analysis [Proton_VX_moment]
Statistical moments of the ion velocity distribution function (VDF) are estimated analytically from the ion current distribution function (CDF).
- Proton velocity component Vy (GSE, km/s) from moment analysis [Proton_VY_moment]
Statistical moments of the ion velocity distribution function (VDF) are estimated analytically from the ion current distribution function (CDF).
- Proton velocity component Vz (GSE, km/s) from moment analysis [Proton_VZ_moment]
Statistical moments of the ion velocity distribution function (VDF) are estimated analytically from the ion current distribution function (CDF).
- Proton thermal speed W (km/s) from isotropic moment analysis [Proton_W_moment]
Statistical moments of the ion velocity distribution function (VDF) are estimated analytically from the ion current distribution function (CDF).
- Proton thermal speed Wperpendicular (km/s) from bimax moment analysis [Proton_Wperp_moment]
Statistical moments of the ion velocity distribution function (VDF) are estimated analytically from the ion current distribution function (CDF).
- Proton thermal speed Wparallel (km/s) from bimax moment analysis [Proton_Wpar_moment]
Statistical moments of the ion velocity distribution function (VDF) are estimated analytically from the ion current distribution function (CDF).
- Proton number density Np (n/cc) from moment analysis [Proton_Np_moment]
Statistical moments of the ion velocity distribution function (VDF) are estimated analytically from the ion current distribution function (CDF).
- ---> Proton number density Np (n/cc) from moment analysis (log scale) [Proton_Np_moment_log]
Statistical moments of the ion velocity distribution function (VDF) are estimated analytically from the ion current distribution function (CDF).
- Magnetic field component Bx (GSE, nT) averaged over plasma measurement [BX]
calculated from 3-second MFI experiment Version 5 data
- Magnetic field component By (GSE, nT) averaged over plasma measurement [BY]
calculated from 3-second MFI experiment Version 5 data
- Magnetic field component Bz (GSE, nT) averaged over plasma measurement [BZ]
calculated from 3-second MFI experiment Version 5 data
- Angluar deviation of magnetic field over plasma measurement [degrees] [Ang_dev]
calculated from 3-second MFI experiment Version 5 data
- Deviation in magnitude of field over plasma measurement [nT] [dev]
calculated from 3-second MFI experiment Version 5 data
- X (GSE) Position of Wind S/C at start of spectrum [Re] [xgse]
- Y (GSE) Position of Wind S/C at start of spectrum [Re] [ygse]
- Z (GSE) Position of Wind S/C at start of spectrum [Re] [zgse]
- Y (GSM) Position of Wind S/C at start of spectrum [Re] [ygsm]
- Z (GSM) Position of Wind S/C at start of spectrum [Re] [zgsm]
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- WI_H1_SWE_RTN
- Description
Notes: - Data reported within this file do not exceed the limits of various paremeters listed in the following section. There may be more valid data in the original dataset that requires additional work to interpret but was discarded due to the limits. In particular we have tried to exclude non-solar wind data and questionable alpha data from these files. - We provide the one sigma uncertainty for each parameter produced by the non-linear curve fitting analysis either directly from the fitting or by propagating uncertainties for bulk speeds, flow angles or any other derived parameter. - For the non-linear anisotropic proton analysis, a scalar thermal speed is produced by determining parallel and perpendicular tmperatures, taking the trace, Tscalar = (2Tperp + Tpara)/3 and converting the result back to a thermal speed. The uncertainties are also propagated through ; Limits: ; Minimum mach number: 1.5000000 ; Maximum chisq/dof: 100000.00 ; Minimum distance ; to bow shock: 5.0000000 [Re] ; Maximum uncertainty in any ; parameter from non-linear ; analysis: 70.0000[%] - Modification History
data analysis package revised March, 2012. RTN Initial Release: July 16 2024
- Data Variable Descriptions
- This flag denotes the fit quality and encodes any contingencies in the ion VDF analysis (10=SW parameters OK) [fit_flag]
FLAG values indicate analysis contingencies: 10: Solar wind parameters OK -- no action necessary 9: Alpha particles relatively too cold 8: Alpha particles overlap within protons in CDF. 7: Alphas too fast, out of SWE range 6: Alpha particle peak may be confused with second proton peak. 5: Parameters OK, but Tp=Ta constraint used (params obtained with SUB_PROT=1) 4: alphas are unusually cold, Tp=Ta constraint used (SUB_PROT=1) 3: alpha patr. relatively too hot (SUB_PROT=1). Tp=Ta constraint used 2: The speed of the alpha is unusually low. 1: Poor peak identification 0: Spectrum cannot be fit with a bimax model.
- ---> year [year]
- ---> Fractional day of year of start of spectrum (Noon on January 1 = 1.5) [doy]
- Proton bulk speed [Proton_V_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- --> Proton bulk speed (w/ uncertainties) [Proton_V_nonlin_errorbars]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> 1-sigma uncertainty of the proton bulk speed [Proton_sigmaV_nonlin]
From fit uncertainty, measurement uncertainties
- R_RTN component of the proton vector velocity [km/s], from non-linear analysis [Proton_VR_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> R_RTN component (with uncertainties) [Proton_VR_nonlin_errorbars]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> 1-sigma uncertainty of measured R_RTN [Proton_sigmaVR_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- T_RTN component of the proton vector velocity [km/s], from non-linear analysis [Proton_VT_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> T_RTN component (with uncertainties) [Proton_VT_nonlin_errorbars]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> 1-sigma uncertainty of measured T_RTN [Proton_sigmaVT_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- N_RTN component of the proton vector velocity [km/s], from non-linear analysis [Proton_VN_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> N_RTN (with uncertainties) [Proton_VN_nonlin_errorbars]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> 1-sigma uncertainty of measured N_RTN [Proton_sigmaVN_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- Scalar [isotropic] proton thermal speed [km/s], from the trace of the anisotropic temperatures. [Proton_W_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> Scalar [isotropic] proton thermal speed (with uncertainties) [Proton_W_nonlin_errorbars]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> 1-sigma uncertainty in the proton trace thermal speed [km/s]. [Proton_sigmaW_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- Proton thermal speed perpendicular to the magnetic field direction [km/s]. [Proton_Wperp_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> Proton thermal speed perpendicular (with uncertainties) [Proton_Wperp_nonlin_errorbars]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> 1-sigma uncertainty in the perpendicular proton thermal speed [km/s]. [Proton_sigmaWperp_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- Proton thermal speed parallel to the magnetic field direction [km/s]. [Proton_Wpar_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> Proton thermal speed (with uncertainties) [Proton_Wpar_nonlin_errorbars]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> 1-sigma uncertainty in the parallel proton thermal speed [km/s]. [Proton_sigmaWpar_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- East-West RTN bulk Flow Angle [degrees] [EW_flowangle]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> East-West RTN bulk Flow Angle (with uncertainties) [EW_flowangle_errorbars]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> 1-sigma uncertainty in the east-west flow angle [SigmaEW_flowangle]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- North-south RTN bulk flow angle [degrees] [NS_flowangle]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> North-south RTN bulk flow angle (with uncertainties) [NS_flowangle_errorbars]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> 1-sigma uncertainty in north-south flow angle [SigmaNS_flowangle]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- Proton number density Np (n/cc) from non-linear analysis (linear scale) [Proton_Np_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> Proton number density Np (log scale) [Proton_Np_nonlin_log]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> Proton number density Np (with uncertainties) [Proton_Np_nonlin_errorbars]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> 1-sigma uncertainty in the proton density [Proton_sigmaNp_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- Alpha bulk speed V (km/s) from non-linear analysis [Alpha_V_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> Alpha bulk speed V (km/s) (with uncertainties) [Alpha_V_nonlin_errorbars]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> 1-sigma uncertainty in alpha V [km/s] [Alpha_sigmaV_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- Alpha velocity component Vr (RTN, km/s) from non-linear analysis [Alpha_VR_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> Alpha velocity component Vr (with uncertainties [Alpha_VR_nonlin_errorbars]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- --->1-sigma uncertainty in alpha Vr [km/s] [Alpha_sigmaVR_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- Alpha velocity component Vt (RTN, km/s) from non-linear analysis [Alpha_VT_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> Alpha velocity component Vt (with uncertainties) [Alpha_VT_nonlin_errorbars]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> 1-sigma uncertainty in alpha Vt [km/s] [Alpha_sigmaVT_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- Alpha velocity component Vn (RTN, km/s) from non-linear analysis [Alpha_VN_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> Alpha velocity component Vn (with uncertainties) [Alpha_VN_nonlin_errorbars]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> 1-sigma uncertainty in alpha Vn [km/s] [Alpha_sigmaVN_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- Scalar [isotropic] alpha particle thermal speed [km/s]. [Alpha_W_nonlin]
Calculated from the trace of the anisotropic alpha pressure tensor, obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> Scalar [isotropic] alpha particle thermal speed [km/s] (with uncertainties). [Alpha_W_nonlin_errorbars]
Calculated from the trace of the anisotropic alpha pressure tensor, obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> 1-sigma uncertainty in trace thermal speed [km/s]. [Alpha_sigmaW_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- Alpha particle thermal speed perpendicular to the magnetic field direction [km/s]. [Alpha_Wperp_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> Alpha particle thermal speed perpendicular to the magnetic field direction [km/s] (with uncertainties) [Alpha_Wperp_nonlin_errorbars]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> 1-sigma uncertainty in the perpendicular alpha thermal speed [km/s]. [Alpha_sigmaWperp_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- Alpha particle thermal speed parallel to the magnetic field direction [km/s] [Alpha_Wpar_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> Alpha particle thermal speed parallel (with uncertainties) [Alpha_Wpar_nonlin_errorbars]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> 1-sigma uncertainty in the perpendicular alpha thermal speed [km/s]. [Alpha_sigmaWpar_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- Alpha number density Na (n/cc) from non-linear analysis [Alpha_Na_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> Alpha number density Na (log scale) [Alpha_Na_nonlin_log]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> Alpha number density Na (with uncertainties) [Alpha_Na_nonlin_errorbars]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> 1-sigma uncertainty in the alpha density [n/cc] [Alpha_sigmaNa_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- Reduced chi-squared for this fit [ChisQ_DOF_nonlin]
Obtained from non-linear fitting to the ion current distribution function (CDF).
- ---> Time that the peak charge flux was observed for each spectrum (in fractional day of year) [Peak_doy]
Statistical moments of the ion velocity distribution function (VDF) are estimated analytically from the ion current distribution function (CDF).
- ---> 1-sigma uncertainty in time of peak flux (in fractional day of year) [sigmaPeak_doy]
calculated from the number of spacecraft spins corresponding to the half-width measurement
- Proton bulk speed (km/s) from moment analysis [Proton_V_moment]
Statistical moments of the ion velocity distribution function (VDF) are estimated analytically from the ion current distribution function (CDF).
- Proton velocity component Vr (RTN, km/s) from moment analysis [Proton_VR_moment]
Statistical moments of the ion velocity distribution function (VDF) are estimated analytically from the ion current distribution function (CDF).
- Proton velocity component Vt (RTN, km/s) from moment analysis [Proton_VT_moment]
Statistical moments of the ion velocity distribution function (VDF) are estimated analytically from the ion current distribution function (CDF).
- Proton velocity component Vn (RTN, km/s) from moment analysis [Proton_VN_moment]
Statistical moments of the ion velocity distribution function (VDF) are estimated analytically from the ion current distribution function (CDF).
- Proton thermal speed W (km/s) from isotropic moment analysis [Proton_W_moment]
Statistical moments of the ion velocity distribution function (VDF) are estimated analytically from the ion current distribution function (CDF).
- Proton thermal speed Wperpendicular (km/s) from bimax moment analysis [Proton_Wperp_moment]
Statistical moments of the ion velocity distribution function (VDF) are estimated analytically from the ion current distribution function (CDF).
- Proton thermal speed Wparallel (km/s) from bimax moment analysis [Proton_Wpar_moment]
Statistical moments of the ion velocity distribution function (VDF) are estimated analytically from the ion current distribution function (CDF).
- Proton number density Np (n/cc) from moment analysis [Proton_Np_moment]
Statistical moments of the ion velocity distribution function (VDF) are estimated analytically from the ion current distribution function (CDF).
- ---> Proton number density Np (n/cc) from moment analysis (log scale) [Proton_Np_moment_log]
Statistical moments of the ion velocity distribution function (VDF) are estimated analytically from the ion current distribution function (CDF).
- Magnetic field component Br (RTN, nT) averaged over plasma measurement [BR]
calculated from 3-second MFI experiment Version 5 data
- Magnetic field component Bt (RTN, nT) averaged over plasma measurement [BT]
calculated from 3-second MFI experiment Version 5 data
- Magnetic field component Bn (RTN, nT) averaged over plasma measurement [BN]
calculated from 3-second MFI experiment Version 5 data
- Angluar deviation of magnetic field over plasma measurement [degrees] [Ang_dev]
calculated from 3-second MFI experiment Version 5 data
- Deviation in magnitude of field over plasma measurement [nT] [dev]
calculated from 3-second MFI experiment Version 5 data
- X (GSE) Position of Wind S/C at start of spectrum [Re] [xgse]
- Y (GSE) Position of Wind S/C at start of spectrum [Re] [ygse]
- Z (GSE) Position of Wind S/C at start of spectrum [Re] [zgse]
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- WI_H1_WAV doi:10.48322/ys2k-6162
- Description
The Radio and Plasma Wave Investigation on the WIND Spacecraft, Sp.Sci.Rev.,Vol 71, pg, 231-263,1995.
- Modification History
CODED JAN,1999, SARDI
- Data Variable Descriptions
- Normalized receiver average voltage (RAD2, 1075-13825 kHz) [E_VOLTAGE_RAD2]
Working channels are about 20 of total 256 frequency channels. Values for other channels are interpolations
- Normalized receiver average voltage (RAD1, 20-1040 kHz) [E_VOLTAGE_RAD1]
- Normalized receiver average voltage (TNR, 4-245 kHz) [E_VOLTAGE_TNR]
- [NO PLOTS] Daily receiver minimum voltage (RAD2, 1075-13825 kHz, non-zero values show active freqs) [Minimum_voltage_RAD2]
Zero value denotes channel average values are interpolated, not directly measured
- [NO PLOTS] Daily receiver minimum voltage (RAD1, 20-1040 kHz, non-zero values show active freqs) [Minimum_voltage_RAD1]
- [NO PLOTS] Daily receiver minimum voltage (TNR, 4-245 kHz, non-zero values show active freqs) [Minimum_voltage_TNR]
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- WI_H2_MFI doi:10.48322/0v0h-df27
- Description
WIND MFI high-resolution data file. Time resolution varies with instrument mode. Modes 0 & 10, low rate: .184s, high rate: .092s Modes 1 & 11, low rate: Prim .092s Sec 1.84s, high rate: Prim .046s Sec .92s Modes 2 & 12, Same as Modes 1 & 11 Calibration constants are 1 minute averages. WIND MFI Instrument turn on 11/12/1994 Data versions: 03 - Extrapolated Bz correction 04 - Final Bz correction 05 - Final attitude and Bz correction References: 1. Lepping, R. P., et al., The WIND Magnetic Field Investigation, p. 207 in The Global Geospace Mission, ed. by C. T. Russell, Kluwer,1995 2. Panetta, P. (GSFC), GGS WIND MFI Operator's Manual, September 15, 1992. 3. Computer Sciences Corporation, Data Format Control Document (DFCD) Between The International Solar-Terrestrial Physics (ISTP) Program Information Processing Division Ground Data Processing System and The ISTP Mission Investigators, CSC/TR-91/6014, 560-1DFD/0190, July 1992. 4. Behannon, K. W., International Solar Terrestrial Physics (ISTP) Program Investigator Data Analysis Requirements For WIND and GEOTAIL Spacecraft Magnetometer Experiment, September 1987. 5. National Space Science Data Center, CDF User's Guide, Version 2.3.0, October 1, 1992. 6. Mish, W. H., International Solar-Terrestrial Physics (ISTP) Key Parameter Generation Software (KPGS) Standards & Conventions, September 1992. 7. Mish, W. H., IMP F and G Phase I Magnetic Field Analysis, April 1972
- Modification History
10/01/2011 Initial release
- Data Variable Descriptions
- Magnetic field magnitude [BF1]
B field Magnitude
- Magnetic field vector in GSM cartesian coordinates [BGSM]
- Magnetic field vector in GSE cartesian coordinates [BGSE]
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- WI_H3-RTN_MFI doi:10.48322/s1d0-5q92
- Description
WIND MFI Composite data file. This file contains multiple time resolution data. 1 Minute data averages 3 Second data averages 1 Hour data averages WIND MFI Instrument turn on 11/12/1994 Data versions: 03 - Extrapolated Bz correction 04 - Final Bz correction 05 - Final orbit and Bz correction References: 1. Lepping, R. P., et al., The WIND Magnetic Field Investigation, p. 207 in The Global Geospace Mission, ed. by C. T. Russell, Kluwer,1995 2. Panetta, P. (GSFC), GGS WIND MFI Operator's Manual, September 15, 1992. 3. Computer Sciences Corporation, Data Format Control Document (DFCD) Between The International Solar-Terrestrial Physics (ISTP) Program Information Processing Division Ground Data Processing System and The ISTP Mission Investigators, CSC/TR-91/6014, 560-1DFD/0190, July 1992. 4. Behannon, K. W., International Solar Terrestrial Physics (ISTP) Program Investigator Data Analysis Requirements For WIND and GEOTAIL Spacecraft Magnetometer Experiment, September 1987. 5. National Space Science Data Center, CDF User's Guide, Version 2.3.0, October 1, 1992. 6. Mish, W. H., International Solar-Terrestrial Physics (ISTP) Key Parameter Generation Software (KPGS) Standards & Conventions, September 1992. 7. Mish, W. H., IMP F and G Phase I Magnetic Field Analysis, April 1972
- Modification History
03/01/2023 Initial release
- Data Variable Descriptions
- Magnetic field magnitude (1 min) [BF1]
Average of the magnitudes (F1)
- RMS magnitude (1 min) [BRMSF1]
RMS of the magnitudes (F1 RMS)
- Magnetic field vector in RTN cartesian coordinates (1 min) [BRTN]
- RMS vector in RTN coordinates (1 min) [BRMSRTN]
- Magnetic field magnitude (3 sec) [B3F1]
Average of the magnitudes (F1)
- RMS magnitude (3 sec) [B3RMSF1]
RMS of the magnitudes (F1 RMS)
- Magnetic field vector in RTN cartesian coordinates (3 sec) [B3RTN]
- RMS vector in RTN coordinates (3 sec) [B3RMSRTN]
- Magnetic field magnitude (1 hour) [B1F1]
Average of the magnitudes (F1)
- RMS magnitude (1 hour) [B1RMSF1]
RMS of the magnitudes (F1 RMS)
- Magnetic field vector in RTN cartesian coordinates (1 hour) [B1RTN]
- RMS vector in RTN coordinates (1 hour) [B1RMSRTN]
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- WI_H3_SWE doi:10.48322/xdpr-7352
- Description
Explanatory notes: The electron pitch-angle distributions included in this data set are derived from sorting, by pitch (wrt B) and energy, the solar wind electron distributions measured by the Wind/SWE electron instrument (see Ogilvie et al., 'SWE, a comprehensive plasma instrument for the Wind spacecraft', Space Sci. Rev., 71, 55, 1955). Pitch-angle distrubutions, organized by energy, are computed from 9s measurements which are usually separated by one or more 3s spin-periods. These quantities are reliable and citable with caution, meaning that the PI advises that the user should discuss their interpretations with a member of the SWE science team before publishing. The following comments are intended to aid in the use and interpretation of the electron pitch-angle distributions reported in this data set. For each 'energy spectrum', observations are made at 13 energy channels: E = 19.34, 38.68, 58.03, 77.37, 96.71, 116.1, 193.4, 290.1, 425.5, 580.3, 773.7, 1006., and 1238. eV. The observations made at each energy are sorted into pitch-angle bins, six degrees in width, from 0 degrees (flux nearly parallel to B) to 180 degrees (flux nearly anti-parallel with B). A 'spin-averaged' set of observations (aggregated from all pitch-angle bins, each energy) is also reported, one value for each energy channel. The value reported for any bin (including the spin-averaged 'energy bins' is given as a phase-space density, f [#/{cc*(cm/s)^3}], averaged over contributing detectors. The data set reported here contains: f_pitch_E00, f_pitch_E01, f_pitch_E02, f_pitch_E03, f_pitch_E04, f_pitch_E05, f_pitch_E06, f_pitch_E07, f_pitch_E08, f_pitch_E09, f_pitch_E10, f_pitch_E11, f_pitch_E12 (the pitch-angle distributions for each energy channel, with 30 pitch-angle bins for each), and f_pitch_SPA (with 13 spin-averaged energy bins). For reference, the electron speeds (|V|, in cm/s) corresponding to the energy channels used, are reported in this data set. - Modification History
Skeleton created 5/30/2007
- Data Variable Descriptions
- Electron pitch-angle distributions (6 degrees/bin), energy channel 00 (19.34 eV, 2.60e+08 cm/s) [f_pitch_E00]
For the EXX distributions, Ve[XX] gives the corresponding electron speed (cm/s).
- Electron pitch-angle distributions (6 degrees/bin), energy channel 01 (38.68 eV, 3.68e+08 cm/s [f_pitch_E01]
For the EXX distributions, Ve[XX] gives the corresponding electron speed (cm/s).
- Electron pitch-angle distributions (6 degrees/bin), energy channel 02 (58.03 eV, 4.51e+08 cm/s) [f_pitch_E02]
For the EXX distributions, Ve[XX] gives the corresponding electron speed (cm/s).
- Electron pitch-angle distributions (6 degrees/bin), energy channel 03 (77.37 eV, 5.21e+08 cm/s) [f_pitch_E03]
For the EXX distributions, Ve[XX] gives the corresponding electron speed (cm/s).
- Electron pitch-angle distributions (6 degrees/bin), energy channel 04 (96.71 eV, 5.82e+08 cm/s) [f_pitch_E04]
For the EXX distributions, Ve[XX] gives the corresponding electron speed (cm/s).
- Electron pitch-angle distributions (6 degrees/bin), energy channel 05 (116.1 eV, 6.38e+08 cm/s) [f_pitch_E05]
For the EXX distributions, Ve[XX] gives the corresponding electron speed (cm/s).
- Electron pitch-angle distributions (6 degrees/bin), energy channel 06 (193.4 eV, 8.23e+08 cm/s) [f_pitch_E06]
For the EXX distributions, Ve[XX] gives the corresponding electron speed (cm/s).
- Electron pitch-angle distributions (6 degrees/bin), energy channel 07 (290.1 eV, 1.00e+09 cm/s) [f_pitch_E07]
For the EXX distributions, Ve[XX] gives the corresponding electron speed (cm/s).
- Electron pitch-angle distributions (6 degrees/bin), energy channel 08 (425.5 eV, 1.22e+09 cm/s) [f_pitch_E08]
For the EXX distributions, Ve[XX] gives the corresponding electron speed (cm/s).
- Electron pitch-angle distributions (6 degrees/bin), energy channel 09 (580.3 eV, 1.42e+09 cm/s) [f_pitch_E09]
For the EXX distributions, Ve[XX] gives the corresponding electron speed (cm/s).
- Electron pitch-angle distributions (6 degrees/bin), energy channel 10 (773.7 eV, 1.64e+09 cm/s) [f_pitch_E10]
For the EXX distributions, Ve[XX] gives the corresponding electron speed (cm/s).
- Electron pitch-angle distributions (6 degrees/bin), energy channel 11 (1006 eV, 1.87e+09 cm/s) [f_pitch_E11]
For the EXX distributions, Ve[XX] gives the corresponding electron speed (cm/s).
- Electron pitch-angle distributions (6 degrees/bin), energy channel 12 (1238 eV, 2.08e+09 cm/s) [f_pitch_E12]
For the EXX distributions, Ve[XX] gives the corresponding electron speed (cm/s).
- Electron spin-averaged flux, binned by electron speed [f_pitch_SPA]
For each spin-averaged flux value, f_pitch_SPA[i], Ve[i] gives the corresponding electron speed (cm/s).
- Electron spin-averaged flux, binned by energy [f_pitch_SPA_ByE]
For each spin-averaged flux value, f_pitch_SPA[i], Ve[i] gives the corresponding electron speed (cm/s)
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- WI_H4-RTN_MFI doi:10.48322/s1kf-0b54
- Description
WIND MFI high-resolution data file. Time resolution varies with instrument mode. Modes 0 & 10, low rate: .184s, high rate: .092s Modes 1 & 11, low rate: Prim .092s Sec 1.84s, high rate: Prim .046s Sec .92s Modes 2 & 12, Same as Modes 1 & 11 Calibration constants are 1 minute averages. WIND MFI Instrument turn on 11/12/1994 Data versions: 03 - Extrapolated Bz correction 04 - Final Bz correction 05 - Final attitude and Bz correction References: 1. Lepping, R. P., et al., The WIND Magnetic Field Investigation, p. 207 in The Global Geospace Mission, ed. by C. T. Russell, Kluwer,1995 2. Panetta, P. (GSFC), GGS WIND MFI Operator's Manual, September 15, 1992. 3. Computer Sciences Corporation, Data Format Control Document (DFCD) Between The International Solar-Terrestrial Physics (ISTP) Program Information Processing Division Ground Data Processing System and The ISTP Mission Investigators, CSC/TR-91/6014, 560-1DFD/0190, July 1992. 4. Behannon, K. W., International Solar Terrestrial Physics (ISTP) Program Investigator Data Analysis Requirements For WIND and GEOTAIL Spacecraft Magnetometer Experiment, September 1987. 5. National Space Science Data Center, CDF User's Guide, Version 2.3.0, October 1, 1992. 6. Mish, W. H., International Solar-Terrestrial Physics (ISTP) Key Parameter Generation Software (KPGS) Standards & Conventions, September 1992. 7. Mish, W. H., IMP F and G Phase I Magnetic Field Analysis, April 1972
- Modification History
03/01/2023 Initial release
- Data Variable Descriptions
- Magnetic field magnitude [BF1]
- Magnetic field vector in RTN cartesian coordinates [BRTN]
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- WI_H4_SWE doi:10.48322/wx5n-w132
- Description
Explanatory notes: The electron pitch-angle distributions included in this data set are derived from sorting, by pitch (wrt B) and energy, the solar wind electron distributions measured by the Wind/SWE electron instrument (see Ogilvie et al., "SWE, a comprehensive plasma instrument for the Wind spacecraft", Space Sci. Rev., 71, 55, 1955). Pitch-angle distrubutions, organized by energy, are computed from 3s measurements which are spaced either 6s or 12s in time. These quantities are reliable and citable with caution, meaning that the PI advises that the user should discuss their interpretations with a member of the SWE science team before publishing. The following comments are intended to aid in the use and interpretation of the electron pitch-angle distributions reported in this data set. For each 'energy spectrum', observations are made at 16 energy channels ranging from about 10 eV to as much as 3 keV. The exact energies at which observations are made is time-varying, and this data set reports the energy each channel observes (along with the observations themselves) at any time. The observations made at each energy are sorted into pitch-angle bins, six degrees in width, from 0 degrees (flux nearly parallel to B) to 180 degrees (flux nearly anti-parallel with B). A "spin-averaged" set of observations (aggregated from all pitch-angle bins, each energy) is also reported, one value for each energy channel. The value reported for any bin (including the spin-averaged "energy bins") is given as a phase-space density, f [#/{cc*(cm/s)^3}], averaged over contributing detectors. The data set reported here contains: f_pitch_E00, f_pitch_E01, f_pitch_E02, f_pitch_E03, f_pitch_E04, f_pitch_E05, f_pitch_E06, f_pitch_E07, f_pitch_E08, f_pitch_E09, f_pitch_E10, f_pitch_E11, f_pitch_E12, f_pitch_E13, f_pitch_E14, f_pitch_E15 (the pitch-angle distributions for each energy channel, with 30 pitch-angle bins for each), and f_pitch_SPA (with 16 spin-averaged energy bins). For reference, the electron speeds (|V|, in cm/s) corresponding to the energy channels used, are reported in this data set. - Modification History
Skeleton created 12/03/2007
- Data Variable Descriptions
- Electron speed [Ve]
time-varying electron speeds corresponding to fluxes
- --> stack plot of all channels [Ve_stack]
time-varying electron speeds corresponding to fluxes
- Electron energy [eV]
time-varying electron speeds corresponding to fluxes
- --> stack plot of all channels, by energy [eV_stack]
time-varying electron energies corresponding to fluxes
- Electron pitch-angle distributions (6 degrees/bin), energy chanel 00 (time-varying energy value) [f_pitch_E00]
For the EXX distributions, Ve[XX] gives the corresponding electron speed (cm/s).
- Electron pitch-angle distributions (6 degrees/bin), energy chanel 01 (time-varying energy value) [f_pitch_E01]
For the EXX distributions, Ve[XX] gives the corresponding electron speed (cm/s).
- Electron pitch-angle distributions (6 degrees/bin), energy chanel 02 (time-varying energy value) [f_pitch_E02]
For the EXX distributions, Ve[XX] gives the corresponding electron speed (cm/s).
- Electron pitch-angle distributions (6 degrees/bin), energy chanel 03 (time-varying energy value) [f_pitch_E03]
For the EXX distributions, Ve[XX] gives the corresponding electron speed (cm/s).
- Electron pitch-angle distributions (6 degrees/bin), energy chanel 04 (time-varying energy value) [f_pitch_E04]
For the EXX distributions, Ve[XX] gives the corresponding electron speed (cm/s).
- Electron pitch-angle distributions (6 degrees/bin), energy chanel 05 (time-varying energy value) [f_pitch_E05]
For the EXX distributions, Ve[XX] gives the corresponding electron speed (cm/s).
- Electron pitch-angle distributions (6 degrees/bin), energy chanel 06 (time-varying energy value) [f_pitch_E06]
For the EXX distributions, Ve[XX] gives the corresponding electron speed (cm/s).
- Electron pitch-angle distributions (6 degrees/bin), energy chanel 07 (time-varying energy value) [f_pitch_E07]
For the EXX distributions, Ve[XX] gives the corresponding electron speed (cm/s).
- Electron pitch-angle distributions (6 degrees/bin), energy chanel 08 (time-varying energy value) [f_pitch_E08]
For the EXX distributions, Ve[XX] gives the corresponding electron speed (cm/s).
- Electron pitch-angle distributions (6 degrees/bin), energy chanel 09 (time-varying energy value) [f_pitch_E09]
For the EXX distributions, Ve[XX] gives the corresponding electron speed (cm/s).
- Electron pitch-angle distributions (6 degrees/bin), energy chanel 10 (time-varying energy value) [f_pitch_E10]
For the EXX distributions, Ve[XX] gives the corresponding electron speed (cm/s).
- Electron pitch-angle distributions (6 degrees/bin), energy chanel 11 (time-varying energy value) [f_pitch_E11]
For the EXX distributions, Ve[XX] gives the corresponding electron speed (cm/s).
- Electron pitch-angle distributions (6 degrees/bin), energy chanel 12 (time-varying energy value) [f_pitch_E12]
For the EXX distributions, Ve[XX] gives the corresponding electron speed (cm/s).
- Electron pitch-angle distributions (6 degrees/bin), energy chanel 13 (time-varying energy value) [f_pitch_E13]
For the EXX distributions, Ve[XX] gives the corresponding electron speed (cm/s).
- Electron pitch-angle distributions (6 degrees/bin), energy chanel 14 (time-varying energy value) [f_pitch_E14]
For the EXX distributions, Ve[XX] gives the corresponding electron speed (cm/s).
- Electron pitch-angle distributions (6 degrees/bin), energy chanel 15 (time-varying energy value) [f_pitch_E15]
For the EXX distributions, Ve[XX] gives the corresponding electron speed (cm/s).
- Electron spin-averaged flux, binned by energy channel [f_pitch_SPA]
For each spin-averaged flux value, f_pitch_SPA[i], Ve[i] gives the corresponding electron speed (cm/s).
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- WI_H5_SWE doi:10.48322/chaz-z942
- Description
Explanatory notes: The electron moments included in this data set are derived from quadrature integration of the solar wind electron distributions (w/ some fitting) measured by the Wind/SWE electron instrument (see Ogilvie et al., "SWE, a comprehensive plasma instrument for the Wind spacecraft", Space Sci. Rev., 71, 55, 1955). Moments parameters are computed from 9s measurements which are usually separated by one or more 3s spin-periods. These quantities are reliable and citable with caution, meaning that the PI advises that the user should discuss their interpretations with a member of the SWE science team before publishing. The following comments are intended to aid in the use and interpretation of the prime quantities of this data set, the electron density, bulk-velocity and temperature. We compensate for the limited nature of our observations under this instrument mode by combining electron observations with bulk-velocity estimates derived from corresponding ion observations. The (13) energy channels over which observations are made are: E = 19.34, 38.68, 58.03, 77.37, 96.71, 116.1, 193.4, 290.1, 425.5, 580.3, 773.7, 1006., and 1238. eV; f(E,Az,El) [#/{cc*(cm/s)^3}] being obtained for each E, using an 8x6 grid of look-directions (Azimuth x Elevation, with ~45x9 deg. "pixels")--thus constituting an 'electron distribution'. A fitted Maxwellian model supplements the "core" regime of each distribution. N_elec [#/cc] gives the density value derived for the full distribution, while NcElec [#/cc] gives that of the core. U_eGSE and UceGSE [km/s, GSE], resp. supply the full and core bulk-velocity. P_eGSE [erg/cc, GSE] has the [Pxx, Pxy, Pxz, Pyy, Pyz, Pzz] components of the derived pressure-tensor. T_elec and TcElec [K], resp. provide the full and core total-temperatures; W_elec and WcElec [eV] specifying the corresponding thermal-energies. Te_pal, Te_per, TecPal and TecPer [K] give resp. full and core parallel- and perpendicular-temperatures (wrt B), with Te_ani and TecAni [unitless] furnishing the perpendicular/parallel temperature-anisotropies for each regime. Finally, Gyrtrp [unitless] indicates the derived electron gyrotropy. The data set reported here contains: N_elec, NcElec, U_eGSE, UceGSE, P_eGSE, T_elec, TcElec, W_elec, WcElec, Te_pal, Te_per, TecPal, TecPer, Te_ani, TecAni, and Gyrtrp (as described above). - Modification History
Skeleton created 12/03/2009.
- Data Variable Descriptions
- Ne Electron density [N_elec]
Number-density from full solar wind electron distribution, including fitted core.
- Ne core Electron density [NcElec]
Number-density from fitted Maxwellian model supplementing the core regime of observed solar wind electron distribution.
- Ue (GSE, 3 comp.) Electron bulk-velocity [U_eGSE]
Bulk-velocity from full solar wind electron distribution, including fitted core.
- Ue core (GSE, 3 comp.) Electron bulk-velocity [UceGSE]
Bulk-velocity from fitted Maxwellian model supplementing the core regime of observed solar wind electron distribution.
- Pe (GSE, 6 comp.) Electron pressure-tensor [P_eGSE]
Pressure-tensor from full solar wind electron distribution, including fitted core.
- Te Electron total-temperature [T_elec]
Total-temperature from full solar wind electron distribution, including fitted core.
- Te core Electron total-temperature [TcElec]
Total-temperature from fitted Maxwellian model supplementing the core regime of observed solar wind electron distribution.
- We Electron average thermal-energy [W_elec]
Average thermal-energy from full solar wind electron distribution, including fitted core.
- We core Electron average thermal-energy [WcElec]
Average thermal-energy from fitted Maxwellian model supplementing the core regime of observed solar wind electron distribution.
- TePal Electron parallel-temperature [Te_pal]
Parallel-temperature (wrt B) from full solar wind electron distribution, including fitted core.
- TePer Electron perpendicular-temperature [Te_per]
Perpendicular-temperature (wrt B) from full solar wind electron distribution, including fitted core.
- TePal core Electron parallel-temperature [TecPal]
Parallel-temperature (wrt B) from fitted Maxwellian model supplementing the core regime of observed solar wind electron distribution.
- TePer core Electron perpendicular-temperature [TecPer]
Perpendicular-temperature (wrt B) from fitted Maxwellian model supplementing the core regime of observed solar wind electron distribution.
- Aniso_e Electron temperature-anisotropy (TePer/TePal) [Te_ani]
Temperature-anisotropy (Te_per/Te_pal) from full solar wind electron distribution, including fitted core.
- Aniso_e core Electron temperature-anisotropy (TePer_core/TePal_core) [TecAni]
Temperature-anisotropy (TecPer/TecPal) from fitted Maxwellian model supplementing the core regime of observed solar wind electron distribution.
- Gyrtrp_e Electron gyrotropy [Gyrtrp]
Gyrotropy from full solar wind electron distribution, including fitted core.
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- WI_K0_3DP doi:10.48322/kwfz-zk29
- Description
Electron flux energy levels: channel 1: 0.1-.4 keV channel 2: 0.4-1.8 keV channel 3: 1.9-8.0 keV channel 4: 9.0-30 keV channel 5: 20-48 keV channel 6: 43-138 keV channel 7: 127-225 keV Ion flux energy levels: channel 1: 0.07-.21 keV channel 2: 0.25-1.1 keV channel 3: 1.3-7 keV channel 4: 8-30 keV channel 5: 20-58 keV channel 6: 58-126 keV channel 7: 115-400 keV pfu == 1/(cm^2-s-sr-keV) Created : Nov, 1991, for 3dpa kpgs testing Modified: May, 1992, to accomodate Standards and Conventions Modified: Jan, 1993, as suggested by Kessel Modified: Mar, 1993, as suggested by Kessel Modified: Jun 7, 1994, for updated 3dpa telemetry specifications Modified: Jun 9, 1994, as suggested by KITT Modified: Jul 10, 1994 Modified: Apr 3, 1995, particle temperatures from K to eV Modified: jun 12, 1995, particle flux scaling adjustments
- Modification History
version 1.0, october 91 version 1.0.1, summer 92 version 1.0.2, january 93 version 1.1, june 94 version 1.1.1, june 94 version 1.1.2, june 94 version 1.1.3, july 94 version 1.2, april 95 version 05, june 95
- Data Variable Descriptions
- Wind s/c position in GSE coords, 3 comp [sc_position]
- Wind s/c velocity in GSE coord., 3 comp. [sc_velocity]
- Electron Flux at 7 energies (0.1-225 keV) [elect_flux]
pfu=particle flux unit=1/(cm^2-s-sr-keV)
- electron density, scalar [elect_density]
- electron velocity in GSE coord, 3 comp. [elect_vel]
- electron temperature, scalar [elect_temp]
- electron heat flux along magnetic field direction [elect_qdotb]
- Ion flux at 7 energies (.07-400 keV) [ion_flux]
pfu=particle flux unit=1/(cm^2-s-sr-keV)
- ion density, scalar [ion_density]
- ion velocity in GSE coord., 3 comp. [ion_vel]
- ion temperature, scalar [ion_temp]
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- WI_K0_EPA doi:10.48322/x9am-dd03
- Description
The parameters contained in this data set are: low energy He, Oxygen, and Iron fluxes in the range 3.2 to 6.2 keV/n; electron flux in the range 1 to 10 Mev/n; proton flux in two contiguous channels from 19 to 72 Mev/n; He flux in four channels from 19 to 640 keV/n; CNO flux in two channels 80 to 640 keV/n; and Iron flux in two channels 80 to 1050 kev/n. The experiment home page at http://lheawww.gsfc.nasa.gov/docs/gamcosray/lecr/EPACT/epact.html gives more detailed information about the instrument.
- Modification History
Created May 10, 1995 Created May 18, 1995
- Data Variable Descriptions
- He flux (3.2 to 6.2 keV/n) [LEMT1]
- Oxygen flux (3.2 to 6.2 keV/n) [LEMT2]
- Iron flux (3.2 TO 6.2 keV/n) [LEMT3]
- e- flux (1 to 10 MeV/n) [APEB1]
- proton flux (19 to 28 MeV/n) [APEB2]
- proton flux (28 to 72 Mev/n) [APEB3]
- He flux (19 to 28 MeV/n) [APEB4]
- He flux (28 to 72 MeV/n) [APEB5]
- He flux (80 to 160 keV/n) [STEP1]
- He flux (320 to 640 keV/n) [STEP2]
- CNO flux (80 to 160 keV/n) [STEP3]
- CNO flux (320 to 640 keV/n) [STEP4]
- Iron flux (80 to 160 keV/n) [STEP5]
- Iron flux (640 to 1050 keV/n) [STEP6]
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- Data Variable Descriptions
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- WI_K0_MFI doi:10.48322/pxak-n392
- Description
References: 1. Panetta P. (GSFC), GGS WIND MFI Operator's Manual, September 15, 1992. 2. Computer Sciences Corporation, Data Format Control Document (DFCD) Between The International Solar-Terrestrial Physics (ISTP) Program Information Processing Division Ground Data Processing System and The ISTP Mission Investigators, CSC/TR-91/6014, 560-1DFD/0190, July 1992. 3. Behannon, K. W., International Solar Terrestrial Physics (ISTP) Program Investigator Data Analysis Requirements For WIND and GEOTAIL Spacecraft Magnetometer Experiment, September 1987.
- Modification History
Initial Release 7/12/93 Zvar Release 10/24/96 Zvar Update 11/12/96
- Data Variable Descriptions
- Average of the magnitudes [BF1]
- Magnetic Field, component RMS SQRT(RMSX^2 + RMSY^2 + RMSZ^2) [RMS]
- Magnetic Field - Cartesian GSM [BGSMc]
- Magnetic Field - Angular GSM [BGSMa]
- Magnetic Field - Cartesian GSE [BGSEc]
- Magnetic Field - Angular GSE [BGSEa]
- Radial distance from the earth [DIST]
- Wind Position - Cartesian GSM [PGSM]
- Wind Position - Cartesian GSE [PGSE]
- Time axis label: Radial distance from the earth [DISTV]
- Time axis label: Wind Position - Cartesian GSM [PGSMV]
- Time axis label: Wind Position - Cartesian GSE [PGSEV]
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- WI_K0_SMS doi:10.48322/wms0-rv35
- Description
Time is for the start of the averaging interval. Computed are the avg alpha vel; avg C/O abundance ratio; avg carbon ionization temp in million degs K from C+6 & C+5 (using the tbls of Arnaud & Rothenflug, 1985); the avg oxygen ionization temp from O+7 & O+6 in million degs K (using tbls of Arnaud & Rothenflug, 1985) Above avgs are made over 4 hrs. He vel and He kinetic temp are computed every 3 min & are contained in the K1 CDF References: Space Science Reviews 71:79-124, 1995, Kluwer Academic Publishers, Belgium Instrument consist of: Solar Wind Ion Composition Spectrometer (SWICS); high resolution mass spectrometer (MASS); Supra-Thermal Ion Composition Spectrometer (STICS) & common DPU
- Modification History
Version 01 Feb. 1996 - whm
- Data Variable Descriptions
- Average alpha velocity, scalar [Alpha_vel]
- Average alpha velocity, scalar, with error bars [Alpha_vel_errorbars]
- Carbon/Oxygen abundance ratio, scalar [C/O_ratio]
- Carbon/Oxygen abundance ratio, scalar, with error bars [C/O_ratio_errorbars]
- Carbon ionization temperature from C+6 & C+5, scalar [C_ion_temp]
- Carbon ionization temperature from C+6 & C+5, scalar, with error bars [C_ion_temp_errorbars]
- Oxygen ionization temperature from O+7 & O+6, scalar [O_ion_temp]
- Oxygen ionization temperature from O+7 & O+6, scalar, with error bars [O_ion_temp_errorbars]
- Uncertainity (+/-30%) in speed of solar wind, scalar [Alpha_Delta]
- Uncertainty (+/-30%) in C/O abundance ratio, scalar [C/O_Delta]
- Uncertainty (+/- 10%) in C ionization temp from C+6 & C+5 [C_Delta]
- Uncertainity (+/- 10%) in O ionization temp O+7 & O+6 [O_Delta]
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- WI_K0_SPHA doi:10.48322/0qwn-gj84
- Description
To be supplied
- Modification History
12/17/92 - Original Implementation, CCR 87 6/14/94 - CCR ISTP 1852, updated CDHF skeleton to CDF standards - JT 11/9/94 - Correct errors made in ccr 1852. CCR 1884
- Data Variable Descriptions
- Spin phase angle [SPIN_PHASE]
- Average spin rate [AVG_SPIN_RATE]
- Std dev of spin rate [STNDEV_SPIN_RATE]
- Fault level status indicator [FAULT]
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- WI_K0_SWE doi:10.48322/3zky-gy15
- Description
SWE, a comprehensive plasma instrument for the WIND spacecraft, K.W. Ogilvie, et al., Space Sci. Rev., 71, 55-77, 1995 USE OF THE QUALITY VARIABLES: *** Good data is indicated by a quality flag of 0. *** The quality flags for each parameter are given as integers 4 bytes long (integer*4). The individual 'bits' for each quality value are set (or cleared) in the analysis code by adding (or subtracting) a power of 2 as follows: To set the 1st bit, add 1. To set the 2nd bit, add 2, To set the 3rd bit, add 4, To set the 4th bit, add 8, and so on. BIT TO_SET_BIT MEANING 1 +1 = 3 point parabolic fits to proton peaks were not attempted. 2 +2 = non-linear least squares fit was not attempted. 3 +4 = 3 point parabolic fits to proton peaks FAILED. 4 +8 = non-linear least squares fit FAILED. See https://cdaweb.gsfc.nasa.gov/wind_swe_quality.html For the complete guide to the quality flag values. - Modification History
12/28/94, 3/4/96, by Alan J. Lazarus John T. Steinberg Daniel B. Berdichevsky. Skeleton TABLE for plasma CDF SWE keyparameters, dbb, Jan., 1994. Instr. qual. flags validmax setequal to +2147483647, 12/94. Qual. flags format changed to compatible values with new validmax, jts and ajl, 12/94. Processing with instrument science modes 2 and 11 added, jts and dbb, 10/27/95. DICT_KEYs added ajl, 3/4/96. Added quality flag info to TEXT field
- Data Variable Descriptions
- Wind s/c position, 3 comp. in GSE coord. [SC_pos_gse]
- Wind s/c position, 3 comp. in GSM coord. [SC_pos_GSM]
- Wind s/c radial distance to center of Earth, scalar [SC_pos_R]
- Velocity Quality Flag: 0=OK; 2 or 130 = caution; Other values NOT VALID [QF_V]
Velocity Quality Flag: 0=OK; 2=parabolic 3-point fit only; 130=parabolic 3-point fit only, sensor 1 only, N/S angle zero degrees assumed; Other values NOT VALID
- Proton Density Quality Flag: 0=OK; 2 or 130 = caution; Other values NOT VALID [QF_Np]
Proton Density Quality Flag: 0=OK; 2=parabolic 3-point fit only; 130=parabolic 3-point fit only, sensor 1 only, N/S angle zero degrees assumed; Other values NOT VALID
- Solar Wind Velocity in GSE coord., 3 comp. [V_GSE]
- Solar Wind Velocity in GSM coord., 3 comp. [V_GSM]
- Ion Bulk Flow vector in GSE coord., 3 comp. (speed, E/W flow, N/S flow) [V_GSE_p]
- Ion Bulk Flow Speed GSE coord.(log) [V_GSE_plog]
- Solar Wind Most Probable Thermal Speed = sqrt(2kT/M), scalar [THERMAL_SPD]
- Solar Wind Proton Number Density, scalar (linear) [Np]
- Solar Wind Proton Number Density, scalar (log) [Np_l]
- Ion Dynamic Pressure (derived from mNV^2), scalar [Pressure]
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- WI_K0_SWE_RTN
- Description
SWE, a comprehensive plasma instrument for the WIND spacecraft, K.W. Ogilvie, et al., Space Sci. Rev., 71, 55-77, 1995. USE OF THE QUALITY VARIABLES: Quality flags are set in the analysis program that generates the KP data. Previous descriptions of their meaning were out of date. Good data is indicated by a quality flag of 0. The quality flags for each parameter are given as integers 4 bytes long (integer*4). The individual 'bits' for each quality value are set (or cleared) in the analysis code by adding (or subtracting) a power of 2 as follows: To set the 1st bit, add 1. To set the 2nd bit, add 2. To set the 3rd bit, add 4. To set the 4th bit, add 8, and so on. BIT TO_SET_BIT MEANING 1 +1 = 3 point parabolic fits to proton peaks were not attempted. 2 +2 = non-linear least squares fit was not attempted. 3 +4 = 3 point parabolic fits to proton peaks FAILED. 4 +8 = non-linear least squares fit FAILED. (Non-linear fit may be reported as good for protons and, at the same time, not good for alphas.) 5 +16 = Alpha params not valid for reason that the non-linear least squares fit was done for protons only. Not enough good energy channels to do simultaneous alpha fit. (This value applies to iqual_core(5) only.) 6 +32 = analysis code unable to get good value for spin period. 7 +64 = SWE instrument in mode 1 - calibration state. Key parameters not produced this mode, only in mode 1 - science. 8 +128 = 3 point fits done for cup 1 only. Split collector ratio of currents used to get n/s angle. Either cup 2 turned off, or cup 2 densities were low indicating noise associated with vibration. 9 +256 = fewer than 10 fc_blocks in spectrum. Analysis skipped. 10 +512 = Alpha non-linear fit produced values of thermal speed and density that do not seem reasonable. 11 +1024 = 3 point parabolic fits to proton peaks done for cup 2 only. Ratio of currents on split collectors used to get n/s angle. Probably Cup 1 is turned off. 12 +2048 = single width windows. Delta E over E 6/5% instead of the default 13%. 13 +4096 = tracking mode operation 14 +8192 = Limited tracking mode scan (Not a full scan) Comments: Non-linear fits are not done for Key Parameters (KPs), but those parameter values are excellent and should be used to do science; non-linear fits are available, but they have problems which suggest strongly that the KP parameters should be used (see paper by Kasper et al., 'Physics-based tests to identify the accuracy of solar wind ion measurements: A case study with the Wind Faraday Cups', J. Geophys. Res., 111, A03105, doi:101029/2005JA011442. Examples (note that all are even numbers because non-linear fits were not attempted) FLAG Meaning 4098 Tracking mode (4096) full scan + no non-linear (2) 14338 Limited tracking mode (8192) + Tracking mode (4096) See http://cdaweb.gsfc.nasa.gov/wind_swe_quality.html for the complete guide to the quality flag values.
- Modification History
12/28/94, 3/4/96, by Alan J. Lazarus John T. Steinberg Daniel B. Berdichevsky. Skeleton TABLE for plasma CDF SWE keyparameters, dbb, Jan., 1994. Instr. qual. flags validmax setequal to +2147483647, 12/94. Qual. flags format changed to compatible values with new validmax, jts and ajl, 12/94. Processing with instrument science modes 2 and 11 added, jts and dbb, 10/27/95. DICT_KEYs added ajl, 3/4/96. Added quality flag info to TEXT field RTN Initial Release: July 16 2024
- Data Variable Descriptions
- Wind s/c position, 3 comp. in GSE coord. [SC_pos_gse]
- Wind s/c position, 3 comp. in GSM coord. [SC_pos_GSM]
- Wind s/c radial distance to center of Earth, scalar [SC_pos_R]
- Solar Wind Velocity in RTN coord., 3 comp. [V_RTN]
- Ion Bulk Flow vector in RTN coord., 3 comp. (speed, E/W flow, N/S flow) [V_RTN_p]
- Solar Wind Most Probable Thermal Speed = sqrt(2kT/M), scalar [THERMAL_SPD]
- Solar Wind Proton Number Density, scalar [Np]
- Percent of density due to alpha particles [Alpha_Percent]
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- WI_K0_WAV doi:10.48322/mfc5-cc53
- Description
SSR WAVES: The Radio and Plasma Wave Investigation on the WIND Spacecraft, Vol 71, pg 231-263,1995.
- Modification History
CODED MAY 1996, C. MEETRE
- Data Variable Descriptions
- Electric field average intensity in dB above background at 76 log-spaced frequencies (250-9.4e6 Hz). [E_Average]
background subtracted using 3% lower bound across each frequency band for entire day - backgrounds given in variable E_Background. Data taken in spin plane only
- Electron density determined from insitu Fpe 'line' position recognized by a neural network. [Ne]
- Transient electric field antenna max from Time Domain Sampler. 0 indicates no trigger. [E_transient]
- Solar array current minimum for s/c [Sol_min]
Solar array current from s/c HK correlates with photoelectric effect on antennas
- Solar array current maximum for s/c [Sol_max]
Solar array current from s/c HK correlates with photoelectric effect on antennas
- Moon Position, Cartesian GSE coordinates [Moon_pos]
- Time axis label: Moon Position, Cartesian GSE coordinates [Moon_posV]
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- WI_K1-RTN_MFI
- Description
References: 1. Panetta P. (GSFC), GGS WIND MFI Operator's Manual, September 15, 1992. 2. Computer Sciences Corporation, Data Format Control Document (DFCD) Between The International Solar-Terrestrial Physics (ISTP) Program Information Processing Division Ground Data Processing System and The ISTP Mission Investigators, CSC/TR-91/6014, 560-1DFD/0190, July 1992. 3. Behannon, K. W., International Solar Terrestrial Physics (ISTP) Program Investigator Data Analysis Requirements For WIND and GEOTAIL Spacecraft Magnetometer Experiment, September 1987.
- Modification History
Initial Release 7/12/93 Zvar Release 10/24/96 Zvar Update 11/12/96 RTN Initial Release: July 16 2024
- Data Variable Descriptions
- Average of the magnitudes [BF1]
- Magnetic Field - Cartesian RTN [BRTN]
- Magnetic Field - Angular RTN [BRTNa]
- Radial distance from the earth [DIST]
- Wind Position - Cartesian GSM [PGSM]
- Wind Position - Cartesian GSE [PGSE]
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- WI_L2-1HOUR-SEP_EPACT-APE_B doi:10.48322/k50r-er56
- Description
The Energetic Particles: Acceleration, Composition and Transport (EPACT) on Wind APE-B Telescope measures proton fluxes 18.90 to 21.90 MeV energetic particle energy
- Modification History
Initial Release 04/01/17
- Data Variable Descriptions
- ---> H intensity, at 1 energy 18.90-21.90 MeV/nuc (time-series with uncertainties) [flux_H]
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- WI_L2-1HOUR-SEP_EPACT-LEMT doi:10.48322/n0f2-3519
- Description
The EPACT Instrument on Wind LEMT - Low Energy Matrix Telescope measures ion fluxes over the charge range from He through Ni from about 0.1 MeV/nucleon to 30 MeV/nucleon, thus covering energetic particle energy ranges.Exploratory measurements of ultra-heavy species (mass range above Ni) will also be performed
- Modification History
Initial Release 10/20/14
- Data Variable Descriptions
- He intensity, at select energies 2.2-8.5 MeV/nuc (stacked plots) [flux_He_stack]
- ---> He intensity, at 7 energies 2.2-8.5 MeV/nuc (time-series with uncertainties) [flux_He]
- C intensity, at select energies 2.9-11.4 MeV/nuc (stacked plots) [flux_C_stack]
- ---> C intensity, at 7 energies 2.9-11.4 MeV/nuc (time-series with uncertainties) [flux_C]
- O intensity, at select energies 2.9-11.3 MeV/nuc (stacked plots) [flux_O_stack]
- ---> O intensity, at 7 energies 2.9-11.3 MeV/nuc (time-series with uncertainties) [flux_O]
- Ne intensity, at select energies 3.6-11.3 MeV/nuc (stacked plots) [flux_Ne_stack]
- ---> Ne intensity, at 6 energies 3.6-11.3 MeV/nuc (time-series with uncertainties) [flux_Ne]
- Si intensity, at select energies 2.8-11.6 MeV/nuc (stacked plots) [flux_Si_stack]
- ---> Si intensity, at 7 energies 2.8-11.6 MeV/nuc (time-series with uncertainties) [flux_Si]
- Fe intensity, at select energies 2.7-10.9 MeV/nuc (stacked plots) [flux_Fe_stack]
- ---> Fe intensity, at 7 energies 2.7-10.9 MeV/nuc (time-series with uncertainties) [flux_Fe]
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- WI_L2-30MIN_SMS-STICS-AFM-MAGNETOSPHERE doi:10.48322/f2m8-ex57
- Description
The Suprathermal Ion Composition Spectrometer (STICS) is a time of flight (TOF) plasma mass spectrometer, capable of identifying mass and mass per charge for incident ions up to 200 keV/e. It uses an electrostatic analyzer to admit ions of a particular energy per charge (E/Q) into the TOF chamber. The E/Q voltage is stepped through 32 values, sitting at each value for approximately 24 sec., to measure ions over the full E/Q range of 6 - 200 keV/e. Ions then pass through a carbon foil and TOF chamber, before finally impacting on a solid-state detector (SSD) for energy measurement. STICS combines these three measurements of E/Q, TOF and residual energy, producing PHA words. This triple-coincidence technique greatly improves the signal to noise ratio in the data. Measurements of E/Q and TOF without residual energy also produce PHA words. These double-coincidence measurements are characterized by better statistics since ions whose energy does not allow them to be registered by the SSD can still be counted in double-coincidence measurements. However, ion identification in double-coincidence measurements are limited to a select number of ions that are well separated in E/Q - TOF space. The STICS instrument provides full 3D velocity distribution functions, through a combination of multiple telescopes and spacecraft spin. The instrument includes 3 separate TOF telescopes that view 3 separate latitude sectors, as shown in Figure 1. In addition, the WIND spacecraft spins, allowing the 3 telescopes to trace out a nearly 4�° steradian viewing area. The longitudinal sectors are shown in Figure 2. The solar direction is in sectors 8-10 while the earthward direction is in sectors 0-2.
- Modification History
Initial release
- Data Variable Descriptions
- Angular flux map triple coincidence H+ [AFM_tc_hplus]
- Angular flux map triple coincidence He+ [AFM_tc_heplus]
- Angular flux map triple coincidence He2+ [AFM_tc_he2plus]
- Angular flux map triple coincidence O+ [AFM_tc_oplus]
- Angular flux map triple coincidence O6+ [AFM_tc_o6plus]
- Angular flux map triple coincidence C5+ [AFM_tc_c5plus]
- Angular flux map triple coincidence Fe10+ [AFM_tc_fe10plus]
- Angular flux map double coincidence H+ [AFM_dc_hplus]
- Angular flux map double coincidence He+ [AFM_dc_heplus]
- Angular flux map double coincidence He2+ [AFM_dc_he2plus]
- Angular flux map double coincidence O+ [AFM_dc_oplus]
- Angular flux map double coincidence O6+ [AFM_dc_o6plus]
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- WI_L2-30MIN_SMS-STICS-AFM-SOLARWIND doi:10.48322/57np-qg69
- Description
The Suprathermal Ion Composition Spectrometer (STICS) is a time of flight (TOF) plasma mass spectrometer, capable of identifying mass and mass per charge for incident ions up to 200 keV/e. It uses an electrostatic analyzer to admit ions of a particular energy per charge (E/Q) into the TOF chamber. The E/Q voltage is stepped through 32 values, sitting at each value for approximately 24 sec., to measure ions over the full E/Q range of 6 - 200 keV/e. Ions then pass through a carbon foil and TOF chamber, before finally impacting on a solid-state detector (SSD) for energy measurement. STICS combines these three measurements of E/Q, TOF and residual energy, producing PHA words. This triple-coincidence technique greatly improves the signal to noise ratio in the data. Measurements of E/Q and TOF without residual energy also produce PHA words. These double-coincidence measurements are characterized by better statistics since ions whose energy does not allow them to be registered by the SSD can still be counted in double-coincidence measurements. However, ion identification in double-coincidence measurements are limited to a select number of ions that are well separated in E/Q - TOF space. The STICS instrument provides full 3D velocity distribution functions, through a combination of multiple telescopes and spacecraft spin. The instrument includes 3 separate TOF telescopes that view 3 separate latitude sectors, as shown in Figure 1. In addition, the WIND spacecraft spins, allowing the 3 telescopes to trace out a nearly 4�° steradian viewing area. The longitudinal sectors are shown in Figure 2. The solar direction is in sectors 8-10 while the earthward direction is in sectors 0-2.
- Modification History
Initial release
- Data Variable Descriptions
- Angular flux map gives the flux of ions flowing in a given direction in triple coincidence H+ [AFM_tc_hplus]
- Angular flux map gives the flux of ions flowing in a given direction in triple coincidence He+ [AFM_tc_heplus]
- Angular flux map gives the flux of ions flowing in a given direction in triple coincidence He2+ [AFM_tc_he2plus]
- Angular flux map gives the flux of ions flowing in a given direction in triple coincidence O+ [AFM_tc_oplus]
- Angular flux map gives the flux of ions flowing in a given direction in triple coincidence O6+ [AFM_tc_o6plus]
- Angular flux map gives the flux of ions flowing in a given direction in triple coincidence C5+ [AFM_tc_c5plus]
- Angular flux map gives the flux of ions flowing in a given direction in triple coincidence Fe10+ [AFM_tc_fe10plus]
- Angular flux map gives the flux of ions flowing in a given direction in double coincidence H+ [AFM_dc_hplus]
- Angular flux map gives the flux of ions flowing in a given direction in double coincidence He+ [AFM_dc_heplus]
- Angular flux map gives the flux of ions flowing in a given direction in double coincidence He2+ [AFM_dc_he2plus]
- Angular flux map gives the flux of ions flowing in a given direction in double coincidence O+ [AFM_dc_oplus]
- Angular flux map gives the flux of ions flowing in a given direction in double coincidence O6+ [AFM_dc_o6plus]
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- WI_L2-30MIN_SMS-STICS-ERPA-MAGNETOSPHERE doi:10.48322/s1x2-0h63
- Description
The Suprathermal Ion Composition Spectrometer (STICS) is a time of flight (TOF) plasma mass spectrometer, capable of identifying mass and mass per charge for incident ions up to 200 keV/e. It uses an electrostatic analyzer to admit ions of a particular energy per charge (E/Q) into the TOF chamber. The E/Q voltage is stepped through 32 values, sitting at each value for approximately 24 sec., to measure ions over the full E/Q range of 6 - 200 keV/e. Ions then pass through a carbon foil and TOF chamber, before finally impacting on a solid-state detector (SSD) for energy measurement. STICS combines these three measurements of E/Q, TOF and residual energy, producing PHA words. This triple-coincidence technique greatly improves the signal to noise ratio in the data. Measurements of E/Q and TOF without residual energy also produce PHA words. These double-coincidence measurements are characterized by better statistics since ions whose energy does not allow them to be registered by the SSD can still be counted in double-coincidence measurements. However, ion identification in double-coincidence measurements are limited to a select number of ions that are well separated in E/Q - TOF space. The STICS instrument provides full 3D velocity distribution functions, through a combination of multiple telescopes and spacecraft spin. The instrument includes 3 separate TOF telescopes that view 3 separate latitude sectors, as shown in Figure 1. In addition, the WIND spacecraft spins, allowing the 3 telescopes to trace out a nearly 4�° steradian viewing area. The longitudinal sectors are shown in Figure 2. The solar direction is in sectors 8-10 while the earthward direction is in sectors 0-2.
- Modification History
Initial release
- Data Variable Descriptions
- Energy-resolved pitch-angle distributions triple coincidence H+ [ERPA_tc_hplus]
- Pitch-angle distributions triple coincidence H+ - summed over energy [ERPA_tc_hplus_sum]
- Energy-resolved pitch-angle distributions triple coincidence He+ [ERPA_tc_heplus]
- Pitch-angle distributions triple coincidence He+ - summed over energy [ERPA_tc_heplus_sum]
- Energy-resolved pitch-angle distributions triple coincidence He2+ [ERPA_tc_he2plus]
- Pitch-angle distributions triple coincidence He2+ - summed over energy [ERPA_tc_he2plus_sum]
- Energy-resolved pitch-angle distributions triple coincidence O+ [ERPA_tc_oplus]
- Pitch-angle distributions triple coincidence O+ - summed over energy [ERPA_tc_oplus_sum]
- Energy-resolved pitch-angle distributions triple coincidence O6+ [ERPA_tc_o6plus]
- Pitch-angle distributions triple coincidence O6+ - summed over energy [ERPA_tc_o6plus_sum]
- Energy-resolved pitch-angle distributions triple coincidence C5+ [ERPA_tc_c5plus]
- Pitch-angle distributions triple coincidence C5+ - summed over energy [ERPA_tc_c5plus_sum]
- Energy-resolved pitch-angle distributions triple coincidence Fe10+ [ERPA_tc_fe10plus]
- Pitch-angle distributions triple coincidence Fe10+ - summed over energy [ERPA_tc_fe10plus_sum]
- Energy-resolved pitch-angle distributions double coincidence H+ [ERPA_dc_hplus]
- Pitch-angle distributions double coincidence H+ - summed over energy [ERPA_dc_hplus_sum]
- Energy-resolved pitch-angle distributions double coincidence He+ [ERPA_dc_heplus]
- Pitch-angle distributions double coincidence He+ - summed over energy [ERPA_dc_heplus_sum]
- Energy-resolved pitch-angle distributions double coincidence He2+ [ERPA_dc_he2plus]
- Pitch-angle distributions double coincidence He2+ - summed over energy [ERPA_dc_he2plus_sum]
- Energy-resolved pitch-angle distributions double coincidence O+ [ERPA_dc_oplus]
- Pitch-angle distributions double coincidence O+ - summed over energy [ERPA_dc_oplus_sum]
- Energy-resolved pitch-angle distributions double coincidence O6+ [ERPA_dc_o6plus]
- Pitch-angle distributions double coincidence O6+ - summed over energy [ERPA_dc_o6plus_sum]
- Energy per charge [eoq]
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-
WI_L2-30MIN_SMS-STICS-ERPA-SOLARWIND doi:10.48322/yd5h-ty18
Proper citations should include the "Accessed on date" in the form . - Description
The Suprathermal Ion Composition Spectrometer (STICS) is a time of flight (TOF) plasma mass spectrometer, capable of identifying mass and mass per charge for incident ions up to 200 keV/e. It uses an electrostatic analyzer to admit ions of a particular energy per charge (E/Q) into the TOF chamber. The E/Q voltage is stepped through 32 values, sitting at each value for approximately 24 sec., to measure ions over the full E/Q range of 6 - 200 keV/e. Ions then pass through a carbon foil and TOF chamber, before finally impacting on a solid-state detector (SSD) for energy measurement. STICS combines these three measurements of E/Q, TOF and residual energy, producing PHA words. This triple-coincidence technique greatly improves the signal to noise ratio in the data. Measurements of E/Q and TOF without residual energy also produce PHA words. These double-coincidence measurements are characterized by better statistics since ions whose energy does not allow them to be registered by the SSD can still be counted in double-coincidence measurements. However, ion identification in double-coincidence measurements are limited to a select number of ions that are well separated in E/Q - TOF space. The STICS instrument provides full 3D velocity distribution functions, through a combination of multiple telescopes and spacecraft spin. The instrument includes 3 separate TOF telescopes that view 3 separate latitude sectors, as shown in Figure 1. In addition, the WIND spacecraft spins, allowing the 3 telescopes to trace out a nearly 4�° steradian viewing area. The longitudinal sectors are shown in Figure 2. The solar direction is in sectors 8-10 while the earthward direction is in sectors 0-2.
- Modification History
Initial release
- Data Variable Descriptions
- Energy-resolved pitch-angle distributions triple coincidence H+ [ERPA_tc_hplus]
- Pitch-angle distributions triple coincidence H+ - summed over energy [ERPA_tc_hplus_sum]
- Energy-resolved pitch-angle distributions triple coincidence He+ [ERPA_tc_heplus]
- Pitch-angle distributions triple coincidence He+ - summed over energy [ERPA_tc_heplus_sum]
- Energy-resolved pitch-angle distributions triple coincidence He2+ [ERPA_tc_he2plus]
- Pitch-angle distributions triple coincidence He2+ - summed over energy [ERPA_tc_he2plus_sum]
- Energy-resolved pitch-angle distributions triple coincidence O+ [ERPA_tc_oplus]
- Pitch-angle distributions triple coincidence O+ - summed over energy [ERPA_tc_oplus_sum]
- Energy-resolved pitch-angle distributions triple coincidence O6+ [ERPA_tc_o6plus]
- Pitch-angle distributions triple coincidence O6+ - summed over energy [ERPA_tc_o6plus_sum]
- Energy-resolved pitch-angle distributions triple coincidence C5+ [ERPA_tc_c5plus]
- Pitch-angle distributions triple coincidence C5+ - summed over energy [ERPA_tc_c5plus_sum]
- Energy-resolved pitch-angle distributions triple coincidence Fe10+ [ERPA_tc_fe10plus]
- Pitch-angle distributions triple coincidence Fe10+ - summed over energy [ERPA_tc_fe10plus_sum]
- Energy-resolved pitch-angle distributions double coincidence H+ [ERPA_dc_hplus]
- Pitch-angle distributions double coincidence H+ - summed over energy [ERPA_dc_hplus_sum]
- Energy-resolved pitch-angle distributions double coincidence He+ [ERPA_dc_heplus]
- Pitch-angle distributions double coincidence He+ - summed over energy [ERPA_dc_heplus_sum]
- Energy-resolved pitch-angle distributions double coincidence He2+ [ERPA_dc_he2plus]
- Pitch-angle distributions double coincidence He2+ - summed over energy [ERPA_dc_he2plus_sum]
- Energy-resolved pitch-angle distributions double coincidence O+ [ERPA_dc_oplus]
- Pitch-angle distributions double coincidence O+ - summed over energy [ERPA_dc_oplus_sum]
- Energy-resolved pitch-angle distributions double coincidence O6+ [ERPA_dc_o6plus]
- Pitch-angle distributions double coincidence O6+ - summed over energy [ERPA_dc_o6plus_sum]
- Energy per charge [eoq]
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- WI_L2-3MIN_SMS-STICS-VDF-MAGNETOSPHERE doi:10.48322/bm5n-eg33
- Description
The Suprathermal Ion Composition Spectrometer (STICS) is a time of flight (TOF) plasma mass spectrometer, capable of identifying mass and mass per charge for incident ions up to 200 keV/e. It uses an electrostatic analyzer to admit ions of a particular energy per charge (E/Q) into the TOF chamber. The E/Q voltage is stepped through 32 values, sitting at each value for approximately 24 sec., to measure ions over the full E/Q range of 6 - 200 keV/e. Ions then pass through a carbon foil and TOF chamber, before finally impacting on a solid-state detector (SSD) for energy measurement. STICS combines these three measurements of E/Q, TOF and residual energy, producing PHA words. This triple-coincidence technique greatly improves the signal to noise ratio in the data. Measurements of E/Q and TOF without residual energy also produce PHA words. These double-coincidence measurements are characterized by better statistics since ions whose energy does not allow them to be registered by the SSD can still be counted in double-coincidence measurements. However, ion identification in double-coincidence measurements are limited to a select number of ions that are well separated in E/Q - TOF space. The STICS instrument provides full 3D velocity distribution functions, through a combination of multiple telescopes and spacecraft spin. The instrument includes 3 separate TOF telescopes that view 3 separate latitude sectors, as shown in Figure 1. In addition, the WIND spacecraft spins, allowing the 3 telescopes to trace out a nearly 4�� steradian viewing area. The longitudinal sectors are shown in Figure 2. The solar direction is in sectors 8-10 while the earthward direction is in sectors 0-2.
- Modification History
Initial release
- Data Variable Descriptions
- [no plot] Full 3-D VDF in phase space density for triple coincidence H+ [DF_tc_hplus]
- Phase space density value triple coincidence H+ - summed over telescope and sector [DF_tc_hplus_sum]
- Phase space density value triple coincidence H+ - summed over telescope and eoq (sorted sector) [DF_tc_hplus_sum1_sort]
SPDF:summed and sorted for spectrogram plot
- Phase space density value triple coincidence H+ (Telescope 2) [DF_T2_tc_hplus]
- [no plot] Error in velocity distribution function value triple coincidence H+ [DF_error_tc_hplus]
- [no plot] Full 3-D VDF in counts for triple coincidence H+ [counts_tc_hplus]
- Counts for triple coincidence H+ - summed over telescope and sector [counts_tc_hplus_sum]
- Counts for triple coincidence H+ - summed over telescope & eoq (sorted sector) [counts_tc_hplus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Counts for triple coincidence H+ (Telescope 2) [counts_T2_tc_hplus]
- [no plot] Error in counts estimated assuming Poisson statistics triple coincidence H+ [counts_error_tc_hplus]
- [no plot] Full 3-D VDF differential flux, dJ/dE triple coincidence H+ [dJ_tc_hplus]
- Differential flux, dJ/dE triple coincidence H+ - summed over telescope and sector [dJ_tc_hplus_sum]
- Differential flux, dJ/dE triple coincidence H+ - summed over telescope and eoq (sorted sector) [dJ_tc_hplus_sum1_sort]
SPDF: summed and sorted for spectrogram
- Differential flux, dJ/dE triple coincidence H+ (Telescope 2) [dJ_T2_tc_hplus]
- [no plot] Error in the differential flux value triple coincidence H+ [dJ_error_tc_hplus]
- [no plot] Full 3-D VDF in phase space density for triple coincidence He+ [DF_tc_heplus]
- Phase space density value triple coincidence He+ - summed over telescope and sector [DF_tc_heplus_sum]
- Phase space density value triple coincidence He+ - summed over telescope and eoq (sorted sector) [DF_tc_heplus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Phase space density value triple coincidence He+ (Telescope 2) [DF_T2_tc_heplus]
- [no plot] Error in velocity distribution function value triple coincidence He+ [DF_error_tc_heplus]
- [no plot] Full 3-D VDF in counts for triple coincidence He+ [counts_tc_heplus]
- Counts for triple coincidence He+ - summed over telescope and sector [counts_tc_heplus_sum]
- Counts for triple coincidence He+ - summed over telescope and eoq (sorted sector) [counts_tc_heplus_sum1_sort]
SPDF:summed and sorted for spectrogram plot
- Counts for triple coincidence He+ (Telescope 2) [counts_T2_tc_heplus]
- [no plot] Error in counts estimated assuming Poisson statistics triple coincidence He+ [counts_error_tc_heplus]
- [no plot] Full 3-D VDF differential flux, dJ/dE triple coincidence He+ [dJ_tc_heplus]
- Differential flux, dJ/dE triple coincidence He+ - summed over telescope and sector [dJ_tc_heplus_sum]
- Differential flux, dJ/dE triple coincidence He+ - summed over telescope and eoq (sorted sector) [dJ_tc_heplus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Differential flux, dJ/dE triple coincidence He+ (Telescope 2) [dJ_T2_tc_heplus]
- [no plot] Error in the differential flux value triple coincidence He+ [dJ_error_tc_heplus]
- [no plot] Full 3-D VDF in phase space density for triple coincidence He2+ [DF_tc_he2plus]
- Phase space density value triple coincidence He2+ - summed over telescope and sector [DF_tc_he2plus_sum]
- Phase space density value triple coincidence He2+ - summed over telescope and eoq (sorted sector) [DF_tc_he2plus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Phase space density value triple coincidence He2+ (Telescope 2) [DF_T2_tc_he2plus]
- [no plot] Error in velocity distribution function value triple coincidence He2+ [DF_error_tc_he2plus]
- [no plot] Full 3-D VDF in counts for triple coincidence He2+ [counts_tc_he2plus]
- Counts for triple coincidence He2+ - summed over telescope and sector [counts_tc_he2plus_sum]
- Counts for triple coincidence He2+ - summed over telescope and eoq (sorted sector) [counts_tc_he2plus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Counts for triple coincidence He2+ (Telescope 2) [counts_T2_tc_he2plus]
- [no plot] Error in counts estimated assuming Poisson statistics triple coincidence He2+ [counts_error_tc_he2plus]
- [no plot] Full 3-D VDF differential flux, dJ/dE triple coincidence He2+ [dJ_tc_he2plus]
- Differential flux, dJ/dE triple coincidence He2+ - summed over telescope and sector [dJ_tc_he2plus_sum]
- Differential flux, dJ/dE triple coincidence He2+ - summed over telescope and eoq (sorted sector) [dJ_tc_he2plus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Differential flux, dJ/dE triple coincidence He2+ (Telescope 2) [dJ_T2_tc_he2plus]
- [no plot] Error in the differential flux value triple coincidence He2+ [dJ_error_tc_he2plus]
- [no plot] Full 3-D VDF in phase space density for triple coincidence O+ [DF_tc_oplus]
- Phase space density value triple coincidence O+ - summed over telescope and sector [DF_tc_oplus_sum]
- Phase space density value triple coincidence O+ - summed over telescope and eoq (sorted sector) [DF_tc_oplus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Phase space density value triple coincidence O+ (Telescope 2) [DF_T2_tc_oplus]
- [no plot] Error in velocity distribution function value triple coincidence O+ [DF_error_tc_oplus]
- [no plot] Full 3-D VDF in counts for triple coincidence O+ [counts_tc_oplus]
- Counts for triple coincidence O+ - summed over telescope and sector [counts_tc_oplus_sum]
- Counts for triple coincidence O+ - summed over telescope & eoq (sorted sector) [counts_tc_oplus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Counts for triple coincidence O+ (Telescope 2) [counts_T2_tc_oplus]
- [no plot] Error in counts estimated assuming Poisson statistics triple coincidence O+ [counts_error_tc_oplus]
- [no plot] Full 3-D VDF differential flux, dJ/dE triple coincidence O+ [dJ_tc_oplus]
- Differential flux, dJ/dE triple coincidence O+ - summed over telescope and sector [dJ_tc_oplus_sum]
- Differential flux, dJ/dE triple coincidence O+ - summed over telescope and eoq (sorted sector) [dJ_tc_oplus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Differential flux, dJ/dE triple coincidence O+ (Telescope 2) [dJ_T2_tc_oplus]
- [no plot] Error in the differential flux value triple coincidence O+ [dJ_error_tc_oplus]
- [no plot] Full 3-D VDF in phase space density for triple coincidence O6+ [DF_tc_o6plus]
- Phase space density value triple coincidence O6+ - summed over telescope and sector [DF_tc_o6plus_sum]
- Phase space density value triple coincidence O6+ - summed over telescope and eoq (sorted sector) [DF_tc_o6plus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Phase space density value triple coincidence O6+ (Telescope 2) [DF_T2_tc_o6plus]
- [no plot] Error in velocity distribution function value triple coincidence O6+ [DF_error_tc_o6plus]
- [no plot] Full 3-D VDF in counts for triple coincidence O6+ [counts_tc_o6plus]
- Counts for triple coincidence O6+ - summed over telescope and sector [counts_tc_o6plus_sum]
- Counts for triple coincidence O6+ - summed over telescope & eoq (sorted sector) [counts_tc_o6plus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Counts for triple coincidence O6+ (Telescope 2) [counts_T2_tc_o6plus]
- [no plot] Error in counts estimated assuming Poisson statistics triple coincidence O6+ [counts_error_tc_o6plus]
- [no plot] Full 3-D VDF differential flux, dJ/dE triple coincidence O6+ [dJ_tc_o6plus]
- Differential flux, dJ/dE triple coincidence O6+ - summed over telescope and sector [dJ_tc_o6plus_sum]
- Differential flux, dJ/dE triple coincidence O6+ - summed over telescope and eoq (sorted sector) [dJ_tc_o6plus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Differential flux, dJ/dE triple coincidence O6+ (Telescope 2) [dJ_T2_tc_o6plus]
- [no plot] Error in the differential flux value triple coincidence O6+ [dJ_error_tc_o6plus]
- [no plot] Full 3-D VDF in phase space density for triple coincidence C5+ [DF_tc_c5plus]
- Phase space density value triple coincidence C5+ - summed over telescope and sector [DF_tc_c5plus_sum]
- Phase space density value triple coincidence C5+ - summed over telescope and eoq (sorted sector) [DF_tc_c5plus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Phase space density value triple coincidence C5+ (Telescope 2) [DF_T2_tc_c5plus]
- [no plot] Error in velocity distribution function value triple coincidence C5+ [DF_error_tc_c5plus]
- [no plot] Full 3-D VDF in counts for triple coincidence C5+ [counts_tc_c5plus]
- Counts for triple coincidence C5+ - summed over telescope and sector [counts_tc_c5plus_sum]
- Counts for triple coincidence C5+ - summed over telescope & eoq (sorted sector) [counts_tc_c5plus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Counts for triple coincidence C5+ (Telescope 2) [counts_T2_tc_c5plus]
- [no plot] Error in counts estimated assuming Poisson statistics triple coincidence C5+ [counts_error_tc_c5plus]
- [no plot] Full 3-D VDF differential flux, dJ/dE triple coincidence C5+ [dJ_tc_c5plus]
- Differential flux, dJ/dE triple coincidence C5+ - summed over telescope and sector [dJ_tc_c5plus_sum]
- Differential flux, dJ/dE triple coincidence C5+ - summed over telescope and eoq (sorted sector) [dJ_tc_c5plus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Differential flux, dJ/dE triple coincidence C5+ (Telescope 2) [dJ_T2_tc_c5plus]
- [no plot] Error in the differential flux value triple coincidence C5+ [dJ_error_tc_c5plus]
- [no plot] Full 3-D VDF in phase space density for triple coincidence Fe10+ [DF_tc_fe10plus]
- Phase space density value triple coincidence Fe10+ - summed over telescope and sector [DF_tc_fe10plus_sum]
- Phase space density value triple coincidence Fe10+ - summed over telescope and eoq (sorted sector) [DF_tc_fe10plus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Phase space density value triple coincidence Fe10+ (Telescope 2) [DF_T2_tc_fe10plus]
- [no plot] Error in velocity distribution function value triple coincidence Fe10+ [DF_error_tc_fe10plus]
- [no plot] Full 3-D VDF in counts for triple coincidence Fe10+ [counts_tc_fe10plus]
- Counts for triple coincidence Fe10+ - summed over telescope and sector [counts_tc_fe10plus_sum]
- Counts for triple coincidence Fe10+ - summed over telescope & eoq (sorted sector) [counts_tc_fe10plus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Counts for triple coincidence Fe10+ (Telescope 2) [counts_T2_tc_fe10plus]
- [no plot] Error in counts estimated assuming Poisson statistics triple coincidence Fe10+ [counts_error_tc_fe10plus]
- [no plot] Full 3-D VDF differential flux, dJ/dE triple coincidence Fe10+ [dJ_tc_fe10plus]
- Differential flux, dJ/dE triple coincidence Fe10+ - summed over telescope and sector [dJ_tc_fe10plus_sum]
- Differential flux, dJ/dE triple coincidence Fe10+ - summed over telescope and eoq (sorted sector) [dJ_tc_fe10plus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Differential flux, dJ/dE triple coincidence Fe10+ (Telescope 2) [dJ_T2_tc_fe10plus]
- [no plot] Error in the differential flux value triple coincidence Fe10+ [dJ_error_tc_fe10plus]
- [no plot] Full 3-D VDF in phase space density for double coincidence H+ [DF_dc_hplus]
- Phase space density value double coincidence H+ - summed over telescope and sector [DF_dc_hplus_sum]
- Phase space density value double coincidence H+ - summed over telescope and eoq (sorted sector) [DF_dc_hplus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Phase space density value double coincidence H+ (Telescope 2) [DF_T2_dc_hplus]
- [no plot] Error in velocity distribution function value double coincidence H+ [DF_error_dc_hplus]
- [no plot] Full 3-D VDF in counts for double coincidence H+ [counts_dc_hplus]
- Counts for double coincidence H+ - summed over telescope and sector [counts_dc_hplus_sum]
- Counts for double coincidence H+ - summed over telescope & eoq (sorted sector) [counts_dc_hplus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Counts for double coincidence H+ (Telescope 2) [counts_T2_dc_hplus]
- [no plot] Error in counts estimated assuming Poisson statistics double coincidence H+ [counts_error_dc_hplus]
- [no plot] Full 3-D VDF differential flux, dJ/dE double coincidence H+ [dJ_dc_hplus]
- Differential flux, dJ/dE double coincidence H+ - summed over telescope and sector [dJ_dc_hplus_sum]
- Differential flux, dJ/dE double coincidence H+ - summed over telescope and eoq (sorted sector) [dJ_dc_hplus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Differential flux, dJ/dE double coincidence H+ (Telescope 2) [dJ_T2_dc_hplus]
- [no plot] Error in the differential flux value double coincidence H+ [dJ_error_dc_hplus]
- [no plot] Full 3-D VDF in phase space density for double coincidence He+ [DF_dc_heplus]
- Phase space density value double coincidence He+ - summed over telescope and sector [DF_dc_heplus_sum]
- Phase space density value double coincidence He+ - summed over telescope and eoq (sorted sector) [DF_dc_heplus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Phase space density value double coincidence He+ (Telescope 2) [DF_T2_dc_heplus]
- [no plot] Error in velocity distribution function value double coincidence He+ [DF_error_dc_heplus]
- [no plot] Full 3-D VDF in counts for double coincidence He+ [counts_dc_heplus]
- Counts for double coincidence He+ - summed over telescope and sector [counts_dc_heplus_sum]
- Counts for double coincidence He+ - summed over telescope & eoq (sorted sector) [counts_dc_heplus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Counts for double coincidence He+ (Telescope 2) [counts_T2_dc_heplus]
- [no plot] Error in counts estimated assuming Poisson statistics double coincidence He+ [counts_error_dc_heplus]
- [no plot] Full 3-D VDF differential flux, dJ/dE double coincidence He+ [dJ_dc_heplus]
- Differential flux, dJ/dE double coincidence He+ - summed over telescope and sector [dJ_dc_heplus_sum]
- Differential flux, dJ/dE double coincidence He+ - summed over telescope and eoq (sorted sector) [dJ_dc_heplus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Differential flux, dJ/dE double coincidence He+ (Telescope 2) [dJ_T2_dc_heplus]
- [no plot] Error in the differential flux value double coincidence He+ [dJ_error_dc_heplus]
- [no plot] Full 3-D VDF in phase space density for double coincidence He2+ [DF_dc_he2plus]
- Phase space density value double coincidence He2+ - summed over telescope and sector [DF_dc_he2plus_sum]
- Phase space density value double coincidence He2+ - summed over telescope and eoq (sorted sector) [DF_dc_he2plus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Phase space density value double coincidence He2+ (Telescope 2) [DF_T2_dc_he2plus]
- [no plot] Error in velocity distribution function value double coincidence He2+ [DF_error_dc_he2plus]
- [no plot] Full 3-D VDF in counts for double coincidence He2+ [counts_dc_he2plus]
- Counts for double coincidence He2+ - summed over telescope and sector [counts_dc_he2plus_sum]
- Counts for double coincidence He2+ - summed over telescope & eoq (sorted sector) [counts_dc_he2plus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Counts for double coincidence He2+ (Telescope 2) [counts_T2_dc_he2plus]
- [no plot] Error in counts estimated assuming Poisson statistics double coincidence He2+ [counts_error_dc_he2plus]
- [no plot] Full 3-D VDF differential flux, dJ/dE double coincidence He2+ [dJ_dc_he2plus]
- Differential flux, dJ/dE double coincidence He2+ - summed over telescope and sector [dJ_dc_he2plus_sum]
- Differential flux, dJ/dE double coincidence He2+ - summed over telescope and eoq (sorted sector) [dJ_dc_he2plus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Differential flux, dJ/dE double coincidence He2+ (Telescope 2) [dJ_T2_dc_he2plus]
- [no plot] Error in the differential flux value double coincidence He2+ [dJ_error_dc_he2plus]
- [no plot] Full 3-D VDF in phase space density for double coincidence O+ [DF_dc_oplus]
- Phase space density value double coincidence O+ - summed over telescope and sector [DF_dc_oplus_sum]
- Phase space density value double coincidence O+ - summed over telescope and eoq (sorted sector) [DF_dc_oplus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Phase space density value double coincidence O+ (Telescope 2) [DF_T2_dc_oplus]
- [no plot] Error in velocity distribution function value double coincidence O+ [DF_error_dc_oplus]
- [no plot] Full 3-D VDF in counts for double coincidence O+ [counts_dc_oplus]
- Counts for double coincidence O+ - summed over telescope and sector [counts_dc_oplus_sum]
- Counts for double coincidence O+ - summed over telescope & eoq (sorted sector) [counts_dc_oplus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Counts for double coincidence O+ (Telescope 2) [counts_T2_dc_oplus]
- [no plot] Error in counts estimated assuming Poisson statistics double coincidence O+ [counts_error_dc_oplus]
- [no plot] Full 3-D VDF differential flux, dJ/dE double coincidence O+ [dJ_dc_oplus]
- Differential flux, dJ/dE double coincidence O+ - summed over telescope and sector [dJ_dc_oplus_sum]
- Differential flux, dJ/dE double coincidence O+ - summed over telescope and eoq (sorted sector) [dJ_dc_oplus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Differential flux, dJ/dE double coincidence O+ (Telescope 2) [dJ_T2_dc_oplus]
- [no plot] Error in the differential flux value double coincidence O+ [dJ_error_dc_oplus]
- [no plot] Full 3-D VDF in phase space density for double coincidence O6+ [DF_dc_o6plus]
- Phase space density value double coincidence O6+ - summed over telescope and sector [DF_dc_o6plus_sum]
- Phase space density value double coincidence O6+ - summed over telescope and eoq (sorted sector) [DF_dc_o6plus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Phase space density value double coincidence O6+ (Telescope 2) [DF_T2_dc_o6plus]
- [no plot] Error in velocity distribution function value double coincidence O6+ [DF_error_dc_o6plus]
- [no plot] Full 3-D VDF in counts for double coincidence O6+ [counts_dc_o6plus]
- Counts for double coincidence O6+ - summed over telescope and sector [counts_dc_o6plus_sum]
- Counts for double coincidence O6+ - summed over telescope & eoq (sorted sector) [counts_dc_o6plus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Counts for double coincidence O6+ (Telescope 2) [counts_T2_dc_o6plus]
- [no plot] Error in counts estimated assuming Poisson statistics double coincidence O6+ [counts_error_dc_o6plus]
- [no plot] Full 3-D VDF differential flux, dJ/dE double coincidence O6+ [dJ_dc_o6plus]
- Differential flux, dJ/dE double coincidence O6+ - summed over telescope and sector [dJ_dc_o6plus_sum]
- Differential flux, dJ/dE double coincidence O6+ - summed over telescope and eoq (sorted sector) [dJ_dc_o6plus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Differential flux, dJ/dE double coincidence O6+ (Telescope 2) [dJ_T2_dc_o6plus]
- [no plot] Error in the differential flux value double coincidence O6+ [dJ_error_dc_o6plus]
- Energy per charge [eoq]
- delta time [delT]
Data Access Code Examples written in
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WI_L2-3MIN_SMS-STICS-VDF-SOLARWIND doi:10.48322/h28x-0w82
Proper citations should include the "Accessed on date" in the form . - Description
The Suprathermal Ion Composition Spectrometer (STICS) is a time of flight (TOF) plasma mass spectrometer, capable of identifying mass and mass per charge for incident ions up to 200 keV/e. It uses an electrostatic analyzer to admit ions of a particular energy per charge (E/Q) into the TOF chamber. The E/Q voltage is stepped through 32 values, sitting at each value for approximately 24 sec., to measure ions over the full E/Q range of 6 - 200 keV/e. Ions then pass through a carbon foil and TOF chamber, before finally impacting on a solid-state detector (SSD) for energy measurement. STICS combines these three measurements of E/Q, TOF and residual energy, producing PHA words. This triple-coincidence technique greatly improves the signal to noise ratio in the data. Measurements of E/Q and TOF without residual energy also produce PHA words. These double-coincidence measurements are characterized by better statistics since ions whose energy does not allow them to be registered by the SSD can still be counted in double-coincidence measurements. However, ion identification in double-coincidence measurements are limited to a select number of ions that are well separated in E/Q - TOF space. The STICS instrument provides full 3D velocity distribution functions, through a combination of multiple telescopes and spacecraft spin. The instrument includes 3 separate TOF telescopes that view 3 separate latitude sectors, as shown in Figure 1. In addition, the WIND spacecraft spins, allowing the 3 telescopes to trace out a nearly 4�� steradian viewing area. The longitudinal sectors are shown in Figure 2. The solar direction is in sectors 8-10 while the earthward direction is in sectors 0-2.
- Modification History
Initial release
- Data Variable Descriptions
- [no plot] Full 3-D VDF in phase space density for triple coincidence H+ [DF_tc_hplus]
- Phase space density value triple coincidence H+ - summed over telescope and sector [DF_tc_hplus_sum]
- Phase space density value triple coincidence H+ - summed over telescope and eoq (sorted sector) [DF_tc_hplus_sum1_sort]
SPDF:summed and sorted for spectrogram plot
- Phase space density value triple coincidence H+ (Telescope 2) [DF_T2_tc_hplus]
- [no plot] Error in velocity distribution function value triple coincidence H+ [DF_error_tc_hplus]
- [no plot] Full 3-D VDF in counts for triple coincidence H+ [counts_tc_hplus]
- Counts for triple coincidence H+ - summed over telescope and sector [counts_tc_hplus_sum]
- Counts for triple coincidence H+ - summed over telescope & eoq (sorted sector) [counts_tc_hplus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Counts for triple coincidence H+ (Telescope 2) [counts_T2_tc_hplus]
- [no plot] Error in counts estimated assuming Poisson statistics triple coincidence H+ [counts_error_tc_hplus]
- [no plot] Full 3-D VDF differential flux, dJ/dE triple coincidence H+ [dJ_tc_hplus]
- Differential flux, dJ/dE triple coincidence H+ - summed over telescope and sector [dJ_tc_hplus_sum]
- Differential flux, dJ/dE triple coincidence H+ - summed over telescope and eoq (sorted sector) [dJ_tc_hplus_sum1_sort]
SPDF: summed and sorted for spectrogram
- Differential flux, dJ/dE triple coincidence H+ (Telescope 2) [dJ_T2_tc_hplus]
- [no plot] Error in the differential flux value triple coincidence H+ [dJ_error_tc_hplus]
- [no plot] Full 3-D VDF in phase space density for triple coincidence He+ [DF_tc_heplus]
- Phase space density value triple coincidence He+ - summed over telescope and sector [DF_tc_heplus_sum]
- Phase space density value triple coincidence He+ - summed over telescope and eoq (sorted sector) [DF_tc_heplus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Phase space density value triple coincidence He+ (Telescope 2) [DF_T2_tc_heplus]
- [no plot] Error in velocity distribution function value triple coincidence He+ [DF_error_tc_heplus]
- [no plot] Full 3-D VDF in counts for triple coincidence He+ [counts_tc_heplus]
- Counts for triple coincidence He+ - summed over telescope and sector [counts_tc_heplus_sum]
- Counts for triple coincidence He+ - summed over telescope and eoq (sorted sector) [counts_tc_heplus_sum1_sort]
SPDF:summed and sorted for spectrogram plot
- Counts for triple coincidence He+ (Telescope 2) [counts_T2_tc_heplus]
- [no plot] Error in counts estimated assuming Poisson statistics triple coincidence He+ [counts_error_tc_heplus]
- [no plot] Full 3-D VDF differential flux, dJ/dE triple coincidence He+ [dJ_tc_heplus]
- Differential flux, dJ/dE triple coincidence He+ - summed over telescope and sector [dJ_tc_heplus_sum]
- Differential flux, dJ/dE triple coincidence He+ - summed over telescope and eoq (sorted sector) [dJ_tc_heplus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Differential flux, dJ/dE triple coincidence He+ (Telescope 2) [dJ_T2_tc_heplus]
- [no plot] Error in the differential flux value triple coincidence He+ [dJ_error_tc_heplus]
- [no plot] Full 3-D VDF in phase space density for triple coincidence He2+ [DF_tc_he2plus]
- Phase space density value triple coincidence He2+ - summed over telescope and sector [DF_tc_he2plus_sum]
- Phase space density value triple coincidence He2+ - summed over telescope and eoq (sorted sector) [DF_tc_he2plus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Phase space density value triple coincidence He2+ (Telescope 2) [DF_T2_tc_he2plus]
- [no plot] Error in velocity distribution function value triple coincidence He2+ [DF_error_tc_he2plus]
- [no plot] Full 3-D VDF in counts for triple coincidence He2+ [counts_tc_he2plus]
- Counts for triple coincidence He2+ - summed over telescope and sector [counts_tc_he2plus_sum]
- Counts for triple coincidence He2+ - summed over telescope and eoq (sorted sector) [counts_tc_he2plus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Counts for triple coincidence He2+ (Telescope 2) [counts_T2_tc_he2plus]
- [no plot] Error in counts estimated assuming Poisson statistics triple coincidence He2+ [counts_error_tc_he2plus]
- [no plot] Full 3-D VDF differential flux, dJ/dE triple coincidence He2+ [dJ_tc_he2plus]
- Differential flux, dJ/dE triple coincidence He2+ - summed over telescope and sector [dJ_tc_he2plus_sum]
- Differential flux, dJ/dE triple coincidence He2+ - summed over telescope and eoq (sorted sector) [dJ_tc_he2plus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Differential flux, dJ/dE triple coincidence He2+ (Telescope 2) [dJ_T2_tc_he2plus]
- [no plot] Error in the differential flux value triple coincidence He2+ [dJ_error_tc_he2plus]
- [no plot] Full 3-D VDF in phase space density for triple coincidence O+ [DF_tc_oplus]
- Phase space density value triple coincidence O+ - summed over telescope and sector [DF_tc_oplus_sum]
- Phase space density value triple coincidence O+ - summed over telescope and eoq (sorted sector) [DF_tc_oplus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Phase space density value triple coincidence O+ (Telescope 2) [DF_T2_tc_oplus]
- [no plot] Error in velocity distribution function value triple coincidence O+ [DF_error_tc_oplus]
- [no plot] Full 3-D VDF in counts for triple coincidence O+ [counts_tc_oplus]
- Counts for triple coincidence O+ - summed over telescope and sector [counts_tc_oplus_sum]
- Counts for triple coincidence O+ - summed over telescope & eoq (sorted sector) [counts_tc_oplus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Counts for triple coincidence O+ (Telescope 2) [counts_T2_tc_oplus]
- [no plot] Error in counts estimated assuming Poisson statistics triple coincidence O+ [counts_error_tc_oplus]
- [no plot] Full 3-D VDF differential flux, dJ/dE triple coincidence O+ [dJ_tc_oplus]
- Differential flux, dJ/dE triple coincidence O+ - summed over telescope and sector [dJ_tc_oplus_sum]
- Differential flux, dJ/dE triple coincidence O+ - summed over telescope and eoq (sorted sector) [dJ_tc_oplus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Differential flux, dJ/dE triple coincidence O+ (Telescope 2) [dJ_T2_tc_oplus]
- [no plot] Error in the differential flux value triple coincidence O+ [dJ_error_tc_oplus]
- [no plot] Full 3-D VDF in phase space density for triple coincidence O6+ [DF_tc_o6plus]
- Phase space density value triple coincidence O6+ - summed over telescope and sector [DF_tc_o6plus_sum]
- Phase space density value triple coincidence O6+ - summed over telescope and eoq (sorted sector) [DF_tc_o6plus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Phase space density value triple coincidence O6+ (Telescope 2) [DF_T2_tc_o6plus]
- [no plot] Error in velocity distribution function value triple coincidence O6+ [DF_error_tc_o6plus]
- [no plot] Full 3-D VDF in counts for triple coincidence O6+ [counts_tc_o6plus]
- Counts for triple coincidence O6+ - summed over telescope and sector [counts_tc_o6plus_sum]
- Counts for triple coincidence O6+ - summed over telescope & eoq (sorted sector) [counts_tc_o6plus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Counts for triple coincidence O6+ (Telescope 2) [counts_T2_tc_o6plus]
- [no plot] Error in counts estimated assuming Poisson statistics triple coincidence O6+ [counts_error_tc_o6plus]
- [no plot] Full 3-D VDF differential flux, dJ/dE triple coincidence O6+ [dJ_tc_o6plus]
- Differential flux, dJ/dE triple coincidence O6+ - summed over telescope and sector [dJ_tc_o6plus_sum]
- Differential flux, dJ/dE triple coincidence O6+ - summed over telescope and eoq (sorted sector) [dJ_tc_o6plus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Differential flux, dJ/dE triple coincidence O6+ (Telescope 2) [dJ_T2_tc_o6plus]
- [no plot] Error in the differential flux value triple coincidence O6+ [dJ_error_tc_o6plus]
- [no plot] Full 3-D VDF in phase space density for triple coincidence C5+ [DF_tc_c5plus]
- Phase space density value triple coincidence C5+ - summed over telescope and sector [DF_tc_c5plus_sum]
- Phase space density value triple coincidence C5+ - summed over telescope and eoq (sorted sector) [DF_tc_c5plus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Phase space density value triple coincidence C5+ (Telescope 2) [DF_T2_tc_c5plus]
- [no plot] Error in velocity distribution function value triple coincidence C5+ [DF_error_tc_c5plus]
- [no plot] Full 3-D VDF in counts for triple coincidence C5+ [counts_tc_c5plus]
- Counts for triple coincidence C5+ - summed over telescope and sector [counts_tc_c5plus_sum]
- Counts for triple coincidence C5+ - summed over telescope & eoq (sorted sector) [counts_tc_c5plus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Counts for triple coincidence C5+ (Telescope 2) [counts_T2_tc_c5plus]
- [no plot] Error in counts estimated assuming Poisson statistics triple coincidence C5+ [counts_error_tc_c5plus]
- [no plot] Full 3-D VDF differential flux, dJ/dE triple coincidence C5+ [dJ_tc_c5plus]
- Differential flux, dJ/dE triple coincidence C5+ - summed over telescope and sector [dJ_tc_c5plus_sum]
- Differential flux, dJ/dE triple coincidence C5+ - summed over telescope and eoq (sorted sector) [dJ_tc_c5plus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Differential flux, dJ/dE triple coincidence C5+ (Telescope 2) [dJ_T2_tc_c5plus]
- [no plot] Error in the differential flux value triple coincidence C5+ [dJ_error_tc_c5plus]
- [no plot] Full 3-D VDF in phase space density for triple coincidence Fe10+ [DF_tc_fe10plus]
- Phase space density value triple coincidence Fe10+ - summed over telescope and sector [DF_tc_fe10plus_sum]
- Phase space density value triple coincidence Fe10+ - summed over telescope and eoq (sorted sector) [DF_tc_fe10plus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Phase space density value triple coincidence Fe10+ (Telescope 2) [DF_T2_tc_fe10plus]
- [no plot] Error in velocity distribution function value triple coincidence Fe10+ [DF_error_tc_fe10plus]
- [no plot] Full 3-D VDF in counts for triple coincidence Fe10+ [counts_tc_fe10plus]
- Counts for triple coincidence Fe10+ - summed over telescope and sector [counts_tc_fe10plus_sum]
- Counts for triple coincidence Fe10+ - summed over telescope & eoq (sorted sector) [counts_tc_fe10plus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Counts for triple coincidence Fe10+ (Telescope 2) [counts_T2_tc_fe10plus]
- [no plot] Error in counts estimated assuming Poisson statistics triple coincidence Fe10+ [counts_error_tc_fe10plus]
- [no plot] Full 3-D VDF differential flux, dJ/dE triple coincidence Fe10+ [dJ_tc_fe10plus]
- Differential flux, dJ/dE triple coincidence Fe10+ - summed over telescope and sector [dJ_tc_fe10plus_sum]
- Differential flux, dJ/dE triple coincidence Fe10+ - summed over telescope and eoq (sorted sector) [dJ_tc_fe10plus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Differential flux, dJ/dE triple coincidence Fe10+ (Telescope 2) [dJ_T2_tc_fe10plus]
- [no plot] Error in the differential flux value triple coincidence Fe10+ [dJ_error_tc_fe10plus]
- [no plot] Full 3-D VDF in phase space density for double coincidence H+ [DF_dc_hplus]
- Phase space density value double coincidence H+ - summed over telescope and sector [DF_dc_hplus_sum]
- Phase space density value double coincidence H+ - summed over telescope and eoq (sorted sector) [DF_dc_hplus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Phase space density value double coincidence H+ (Telescope 2) [DF_T2_dc_hplus]
- [no plot] Error in velocity distribution function value double coincidence H+ [DF_error_dc_hplus]
- [no plot] Full 3-D VDF in counts for double coincidence H+ [counts_dc_hplus]
- Counts for double coincidence H+ - summed over telescope and sector [counts_dc_hplus_sum]
- Counts for double coincidence H+ - summed over telescope & eoq (sorted sector) [counts_dc_hplus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Counts for double coincidence H+ (Telescope 2) [counts_T2_dc_hplus]
- [no plot] Error in counts estimated assuming Poisson statistics double coincidence H+ [counts_error_dc_hplus]
- [no plot] Full 3-D VDF differential flux, dJ/dE double coincidence H+ [dJ_dc_hplus]
- Differential flux, dJ/dE double coincidence H+ - summed over telescope and sector [dJ_dc_hplus_sum]
- Differential flux, dJ/dE double coincidence H+ - summed over telescope and eoq (sorted sector) [dJ_dc_hplus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Differential flux, dJ/dE double coincidence H+ (Telescope 2) [dJ_T2_dc_hplus]
- [no plot] Error in the differential flux value double coincidence H+ [dJ_error_dc_hplus]
- [no plot] Full 3-D VDF in phase space density for double coincidence He+ [DF_dc_heplus]
- Phase space density value double coincidence He+ - summed over telescope and sector [DF_dc_heplus_sum]
- Phase space density value double coincidence He+ - summed over telescope and eoq (sorted sector) [DF_dc_heplus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Phase space density value double coincidence He+ (Telescope 2) [DF_T2_dc_heplus]
- [no plot] Error in velocity distribution function value double coincidence He+ [DF_error_dc_heplus]
- [no plot] Full 3-D VDF in counts for double coincidence He+ [counts_dc_heplus]
- Counts for double coincidence He+ - summed over telescope and sector [counts_dc_heplus_sum]
- Counts for double coincidence He+ - summed over telescope & eoq (sorted sector) [counts_dc_heplus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Counts for double coincidence He+ (Telescope 2) [counts_T2_dc_heplus]
- [no plot] Error in counts estimated assuming Poisson statistics double coincidence He+ [counts_error_dc_heplus]
- [no plot] Full 3-D VDF differential flux, dJ/dE double coincidence He+ [dJ_dc_heplus]
- Differential flux, dJ/dE double coincidence He+ - summed over telescope and sector [dJ_dc_heplus_sum]
- Differential flux, dJ/dE double coincidence He+ - summed over telescope and eoq (sorted sector) [dJ_dc_heplus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Differential flux, dJ/dE double coincidence He+ (Telescope 2) [dJ_T2_dc_heplus]
- [no plot] Error in the differential flux value double coincidence He+ [dJ_error_dc_heplus]
- [no plot] Full 3-D VDF in phase space density for double coincidence He2+ [DF_dc_he2plus]
- Phase space density value double coincidence He2+ - summed over telescope and sector [DF_dc_he2plus_sum]
- Phase space density value double coincidence He2+ - summed over telescope and eoq (sorted sector) [DF_dc_he2plus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Phase space density value double coincidence He2+ (Telescope 2) [DF_T2_dc_he2plus]
- [no plot] Error in velocity distribution function value double coincidence He2+ [DF_error_dc_he2plus]
- [no plot] Full 3-D VDF in counts for double coincidence He2+ [counts_dc_he2plus]
- Counts for double coincidence He2+ - summed over telescope and sector [counts_dc_he2plus_sum]
- Counts for double coincidence He2+ - summed over telescope & eoq (sorted sector) [counts_dc_he2plus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Counts for double coincidence He2+ (Telescope 2) [counts_T2_dc_he2plus]
- [no plot] Error in counts estimated assuming Poisson statistics double coincidence He2+ [counts_error_dc_he2plus]
- [no plot] Full 3-D VDF differential flux, dJ/dE double coincidence He2+ [dJ_dc_he2plus]
- Differential flux, dJ/dE double coincidence He2+ - summed over telescope and sector [dJ_dc_he2plus_sum]
- Differential flux, dJ/dE double coincidence He2+ - summed over telescope and eoq (sorted sector) [dJ_dc_he2plus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Differential flux, dJ/dE double coincidence He2+ (Telescope 2) [dJ_T2_dc_he2plus]
- [no plot] Error in the differential flux value double coincidence He2+ [dJ_error_dc_he2plus]
- [no plot] Full 3-D VDF in phase space density for double coincidence O+ [DF_dc_oplus]
- Phase space density value double coincidence O+ - summed over telescope and sector [DF_dc_oplus_sum]
- Phase space density value double coincidence O+ - summed over telescope and eoq (sorted sector) [DF_dc_oplus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Phase space density value double coincidence O+ (Telescope 2) [DF_T2_dc_oplus]
- [no plot] Error in velocity distribution function value double coincidence O+ [DF_error_dc_oplus]
- [no plot] Full 3-D VDF in counts for double coincidence O+ [counts_dc_oplus]
- Counts for double coincidence O+ - summed over telescope and sector [counts_dc_oplus_sum]
- Counts for double coincidence O+ - summed over telescope & eoq (sorted sector) [counts_dc_oplus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Counts for double coincidence O+ (Telescope 2) [counts_T2_dc_oplus]
- [no plot] Error in counts estimated assuming Poisson statistics double coincidence O+ [counts_error_dc_oplus]
- [no plot] Full 3-D VDF differential flux, dJ/dE double coincidence O+ [dJ_dc_oplus]
- Differential flux, dJ/dE double coincidence O+ - summed over telescope and sector [dJ_dc_oplus_sum]
- Differential flux, dJ/dE double coincidence O+ - summed over telescope and eoq (sorted sector) [dJ_dc_oplus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Differential flux, dJ/dE double coincidence O+ (Telescope 2) [dJ_T2_dc_oplus]
- [no plot] Error in the differential flux value double coincidence O+ [dJ_error_dc_oplus]
- [no plot] Full 3-D VDF in phase space density for double coincidence O6+ [DF_dc_o6plus]
- Phase space density value double coincidence O6+ - summed over telescope and sector [DF_dc_o6plus_sum]
- Phase space density value double coincidence O6+ - summed over telescope and eoq (sorted sector) [DF_dc_o6plus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Phase space density value double coincidence O6+ (Telescope 2) [DF_T2_dc_o6plus]
- [no plot] Error in velocity distribution function value double coincidence O6+ [DF_error_dc_o6plus]
- [no plot] Full 3-D VDF in counts for double coincidence O6+ [counts_dc_o6plus]
- Counts for double coincidence O6+ - summed over telescope and sector [counts_dc_o6plus_sum]
- Counts for double coincidence O6+ - summed over telescope & eoq (sorted sector) [counts_dc_o6plus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Counts for double coincidence O6+ (Telescope 2) [counts_T2_dc_o6plus]
- [no plot] Error in counts estimated assuming Poisson statistics double coincidence O6+ [counts_error_dc_o6plus]
- [no plot] Full 3-D VDF differential flux, dJ/dE double coincidence O6+ [dJ_dc_o6plus]
- Differential flux, dJ/dE double coincidence O6+ - summed over telescope and sector [dJ_dc_o6plus_sum]
- Differential flux, dJ/dE double coincidence O6+ - summed over telescope and eoq (sorted sector) [dJ_dc_o6plus_sum1_sort]
SPDF: summed and sorted for spectrogram plot
- Differential flux, dJ/dE double coincidence O6+ (Telescope 2) [dJ_T2_dc_o6plus]
- [no plot] Error in the differential flux value double coincidence O6+ [dJ_error_dc_o6plus]
- Energy per charge [eoq]
- delta time [delT]
Data Access Code Examples written in
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- WI_L2-5MIN-SEP_EPACT-LEMT doi:10.48322/5jq3-gs16
- Description
The EPACT Instrument on Wind LEMT - Low Energy Matrix Telescope measures ion fluxes over the charge range from He through Ni from about 0.1 MeV/nucleon to 30 MeV/nucleon, thus covering energetic particle energy ranges.Exploratory measurements of ultra-heavy species (mass range above Ni) will also be performed
- Modification History
Initial Release 10/20/14
- Data Variable Descriptions
- Duration [duration]
This number is the number of minutes of the interval since the fluxes are collected
- He intensity, at select energies 2.2-8.5 MeV/nuc (stacked plots) [flux_He_stack]
- ---> He intensity, at 7 energies 2.2-8.5 MeV/nuc (time-series with uncertainties) [flux_He]
- C intensity, at select energies 2.9-11.4 MeV/nuc (stacked plots) [flux_C_stack]
- ---> C intensity, at 7 energies 2.9-11.4 MeV/nuc (time-series with uncertainties) [flux_C]
- O intensity, at select energies 2.9-11.3 MeV/nuc (stacked plots) [flux_O_stack]
- ---> O intensity, at 7 energies 2.9-11.3 MeV/nuc (time-series with uncertainties) [flux_O]
- Ne intensity, at select energies 3.6-11.3 MeV/nuc (stacked plots) [flux_Ne_stack]
- ---> Ne intensity, at 6 energies 3.6-11.3 MeV/nuc (time-series with uncertainties) [flux_Ne]
- Si intensity, at select energies 2.8-11.6 MeV/nuc (stacked plots) [flux_Si_stack]
- ---> Si intensity, at 7 energies 2.8-11.6 MeV/nuc (time-series with uncertainties) [flux_Si]
- Fe intensity, at select energies 2.7-10.9 MeV/nuc (stacked plots) [flux_Fe_stack]
- ---> Fe intensity, at 7 energies 2.7-10.9 MeV/nuc (time-series with uncertainties) [flux_Fe]
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- WI_L2_3MIN_SMS-STICS-NVT-MAGNETOSPHERE doi:10.48322/wnzt-eh29
- Description
The Suprathermal Ion Composition Spectrometer (STICS) is a time of flight (TOF) plasma mass spectrometer, capable of identifying mass and mass per charge for incident ions up to 200 keV/e. It uses an electrostatic analyzer to admit ions of a particular energy per charge (E/Q) into the TOF chamber. The E/Q voltage is stepped through 32 values, sitting at each value for approximately 24 sec., to measure ions over the full E/Q range of 6 - 200 keV/e. Ions then pass through a carbon foil and TOF chamber, before finally impacting on a solid-state detector (SSD) for energy measurement. STICS combines these three measurements of E/Q, TOF and residual energy, producing PHA words. This triple-coincidence technique greatly improves the signal to noise ratio in the data. Measurements of E/Q and TOF without residual energy also produce PHA words. These double-coincidence measurements are characterized by better statistics since ions whose energy does not allow them to be registered by the SSD can still be counted in double-coincidence measurements. However, ion identification in double-coincidence measurements are limited to a select number of ions that are well separated in E/Q - TOF space. The STICS instrument provides full 3D velocity distribution functions, through a combination of multiple telescopes and spacecraft spin. The instrument includes 3 separate TOF telescopes that view 3 separate latitude sectors, as shown in Figure 1. In addition, the WIND spacecraft spins, allowing the 3 telescopes to trace out a nearly 4�° steradian viewing area. The longitudinal sectors are shown in Figure 2. The solar direction is in sectors 8-10 while the earthward direction is in sectors 0-2.
- Modification History
Initial release
- Data Variable Descriptions
- Density H+ triple coincidence [n_tc_hplus]
- --- Error in the density value assuming Poisson statistics H+ triple coincidence [n_err_tc_hplus]
- Average energy H+ triple coincidence [E_ave_tc_hplus]
- --- Error average energy value H+ triple coincidence [E_ave_err_tc_hplus]
- Density He+ triple coincidence [n_tc_heplus]
- --- Error in the density value assuming Poisson statistics He+ triple coincidence [n_err_tc_heplus]
- Average energy He+ triple coincidence [E_ave_tc_heplus]
- --- Error average energy value He+ triple coincidence [E_ave_err_tc_heplus]
- Density He2+ triple coincidence [n_tc_he2plus]
- --- Error in the density value assuming Poisson statistics He2+ triple coincidence [n_err_tc_he2plus]
- Average energy He2+ triple coincidence [E_ave_tc_he2plus]
- --- Error average energy value He2+ triple coincidence [E_ave_err_tc_he2plus]
- Density O+ triple coincidence [n_tc_oplus]
- --- Error in the density value assuming Poisson statistics O+ triple coincidence [n_err_tc_oplus]
- Average energy O+ triple coincidence [E_ave_tc_oplus]
- --- Error average energy value O+ triple coincidence [E_ave_err_tc_oplus]
- Density O6+ triple coincidence [n_tc_o6plus]
- --- Error in the density value assuming Poisson statistics O6+ triple coincidence [n_err_tc_o6plus]
- Average energy O6+ triple coincidence [E_ave_tc_o6plus]
- --- Error average energy value O6+ triple coincidence [E_ave_err_tc_o6plus]
- Density C5+ triple coincidence [n_tc_c5plus]
- --- Error in the density value assuming Poisson statistics C5+ triple coincidence [n_err_tc_c5plus]
- Average energy C5+ triple coincidence [E_ave_tc_c5plus]
- --- Error average energy value C5+ triple coincidence [E_ave_err_tc_c5plus]
- Density Fe10+ triple coincidence [n_tc_fe10plus]
- --- Error in the density value assuming Poisson statistics Fe10+ triple coincidence [n_err_tc_fe10plus]
- Average energy Fe10+ triple coincidence [E_ave_tc_fe10plus]
- --- Error average energy value Fe10+ triple coincidence [E_ave_err_tc_fe10plus]
- Density H+ double coincidence [n_dc_hplus]
- --- Error in the density value assuming Poisson statistics H+ double coincidence [n_err_dc_hplus]
- Average energy H+ double coincidence [E_ave_dc_hplus]
- --- Error average energy value H+ double coincidence [E_ave_err_dc_hplus]
- Density He+ double coincidence [n_dc_heplus]
- --- Error in the density value assuming Poisson statistics He+ double coincidence [n_err_dc_heplus]
- Average energy He+ double coincidence [E_ave_dc_heplus]
- --- Error average energy value He+ double coincidence [E_ave_err_dc_heplus]
- Density He2+ double coincidence [n_dc_he2plus]
- --- Error in the density value assuming Poisson statistics He2+ double coincidence [n_err_dc_he2plus]
- Average energy He2+ double coincidence [E_ave_dc_he2plus]
- --- Error average energy value He2+ double coincidence [E_ave_err_dc_he2plus]
- Density O+ double coincidence [n_dc_oplus]
- --- Error in the density value assuming Poisson statistics O+ double coincidence [n_err_dc_oplus]
- Average energy O+ double coincidence [E_ave_dc_oplus]
- --- Error average energy value O+ double coincidence [E_ave_err_dc_oplus]
- Density O6+ double coincidence [n_dc_o6plus]
- --- Error in the density value assuming Poisson statistics O6+ double coincidence [n_err_dc_o6plus]
- Average energy O6+ double coincidence [E_ave_dc_o6plus]
- --- Error average energy value O6+ double coincidence [E_ave_err_dc_o6plus]
- delta time [delT]
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- WI_L2_3MIN_SMS-STICS-NVT-SOLARWIND doi:10.48322/2mh5-qw88
- Description
The Suprathermal Ion Composition Spectrometer (STICS) is a time of flight (TOF) plasma mass spectrometer, capable of identifying mass and mass per charge for incident ions up to 200 keV/e. It uses an electrostatic analyzer to admit ions of a particular energy per charge (E/Q) into the TOF chamber. The E/Q voltage is stepped through 32 values, sitting at each value for approximately 24 sec., to measure ions over the full E/Q range of 6 - 200 keV/e. Ions then pass through a carbon foil and TOF chamber, before finally impacting on a solid-state detector (SSD) for energy measurement. STICS combines these three measurements of E/Q, TOF and residual energy, producing PHA words. This triple-coincidence technique greatly improves the signal to noise ratio in the data. Measurements of E/Q and TOF without residual energy also produce PHA words. These double-coincidence measurements are characterized by better statistics since ions whose energy does not allow them to be registered by the SSD can still be counted in double-coincidence measurements. However, ion identification in double-coincidence measurements are limited to a select number of ions that are well separated in E/Q - TOF space. The STICS instrument provides full 3D velocity distribution functions, through a combination of multiple telescopes and spacecraft spin. The instrument includes 3 separate TOF telescopes that view 3 separate latitude sectors, as shown in Figure 1. In addition, the WIND spacecraft spins, allowing the 3 telescopes to trace out a nearly 4�° steradian viewing area. The longitudinal sectors are shown in Figure 2. The solar direction is in sectors 8-10 while the earthward direction is in sectors 0-2.
- Modification History
Initial release
- Data Variable Descriptions
- Density H+ triple coincidence [n_tc_hplus]
- --- Error in the density value assuming Poisson statistics H+ triple coincidence [n_err_tc_hplus]
- Average energy H+ triple coincidence [E_ave_tc_hplus]
- --- Error average energy value H+ triple coincidence [E_ave_err_tc_hplus]
- Density He+ triple coincidence [n_tc_heplus]
- --- Error in the density value assuming Poisson statistics He+ triple coincidence [n_err_tc_heplus]
- Average energy He+ triple coincidence [E_ave_tc_heplus]
- --- Error average energy value He+ triple coincidence [E_ave_err_tc_heplus]
- Density He2+ triple coincidence [n_tc_he2plus]
- --- Error in the density value assuming Poisson statistics He2+ triple coincidence [n_err_tc_he2plus]
- Average energy He2+ triple coincidence [E_ave_tc_he2plus]
- --- Error average energy value He2+ triple coincidence [E_ave_err_tc_he2plus]
- Density O+ triple coincidence [n_tc_oplus]
- --- Error in the density value assuming Poisson statistics O+ triple coincidence [n_err_tc_oplus]
- Average energy O+ triple coincidence [E_ave_tc_oplus]
- --- Error average energy value O+ triple coincidence [E_ave_err_tc_oplus]
- Density O6+ triple coincidence [n_tc_o6plus]
- --- Error in the density value assuming Poisson statistics O6+ triple coincidence [n_err_tc_o6plus]
- Average energy O6+ triple coincidence [E_ave_tc_o6plus]
- --- Error average energy value O6+ triple coincidence [E_ave_err_tc_o6plus]
- Density C5+ triple coincidence [n_tc_c5plus]
- --- Error in the density value assuming Poisson statistics C5+ triple coincidence [n_err_tc_c5plus]
- Average energy C5+ triple coincidence [E_ave_tc_c5plus]
- --- Error average energy value C5+ triple coincidence [E_ave_err_tc_c5plus]
- Density Fe10+ triple coincidence [n_tc_fe10plus]
- --- Error in the density value assuming Poisson statistics Fe10+ triple coincidence [n_err_tc_fe10plus]
- Average energy Fe10+ triple coincidence [E_ave_tc_fe10plus]
- --- Error average energy value Fe10+ triple coincidence [E_ave_err_tc_fe10plus]
- Density H+ double coincidence [n_dc_hplus]
- --- Error in the density value assuming Poisson statistics H+ double coincidence [n_err_dc_hplus]
- Average energy H+ double coincidence [E_ave_dc_hplus]
- --- Error average energy value H+ double coincidence [E_ave_err_dc_hplus]
- Density He+ double coincidence [n_dc_heplus]
- --- Error in the density value assuming Poisson statistics He+ double coincidence [n_err_dc_heplus]
- Average energy He+ double coincidence [E_ave_dc_heplus]
- --- Error average energy value He+ double coincidence [E_ave_err_dc_heplus]
- Density He2+ double coincidence [n_dc_he2plus]
- --- Error in the density value assuming Poisson statistics He2+ double coincidence [n_err_dc_he2plus]
- Average energy He2+ double coincidence [E_ave_dc_he2plus]
- --- Error average energy value He2+ double coincidence [E_ave_err_dc_he2plus]
- Density O+ double coincidence [n_dc_oplus]
- --- Error in the density value assuming Poisson statistics O+ double coincidence [n_err_dc_oplus]
- Average energy O+ double coincidence [E_ave_dc_oplus]
- --- Error average energy value O+ double coincidence [E_ave_err_dc_oplus]
- Density O6+ double coincidence [n_dc_o6plus]
- --- Error in the density value assuming Poisson statistics O6+ double coincidence [n_err_dc_o6plus]
- Average energy O6+ double coincidence [E_ave_dc_o6plus]
- --- Error average energy value O6+ double coincidence [E_ave_err_dc_o6plus]
- delta time [delT]
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WI_L2_WAV_RAD1 doi:tbd
Proper citations should include the "Accessed on date" in the form . - Description
This file includes radio measurements recorded by the Wind/WAVES/RAD1 instrument. Time resolution varies with instrument mode ranging from few tenth of seconds to 192 seconds
- Modification History
2022-10-28: Coded by Vratislav Krupar (vratislav.krupar@nasa.gov)
- Data Variable Descriptions
- Power spectral density before antenna calibration (S antenna) [PSD_V2_S]
- Power spectral density before antenna calibration (SP antenna) [PSD_V2_SP]
- Power spectral density before antenna calibration (Z antenna) [PSD_V2_Z]
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WI_L2_WAV_RAD2 doi:tbd
Proper citations should include the "Accessed on date" in the form . - Description
This file includes radio measurements recorded by the Wind/WAVES/RAD2 instrument. Time resolution varies with instrument mode ranging from few tenth of seconds to 192 seconds.
- Modification History
2022-10-28: Coded by Vratislav Krupar (vratislav.krupar@nasa.gov)
- Data Variable Descriptions
- Power spectral density before antenna calibration (S antenna) [PSD_V2_S]
- Power spectral density before antenna calibration (SP antenna) [PSD_V2_SP]
- Power spectral density before antenna calibration (Z antenna) [PSD_V2_Z]
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- WI_L2_WAV_TNR
- Description
This file includes radio measurements recorded by the Wind/WAVES/TNR instrument
- Modification History
2025-09-09: Coded by Vratislav Krupar (vratislav.krupar@nasa.gov)
- Data Variable Descriptions
- Electric field power spectral density [PSD_V2]
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- WI_L3-DUSTIMPACT_WAVES doi:10.48322/635a-nc73
- Description
Wind WAVES Time Domain Sampler (TDS) Dust Data File References: 1) Bougeret, J.-L., et al. `WAVES: The Radio and Plasma Wave Investigation on the Wind Spacecraft,` Space Sci. Rev. Vol. 71, pp. 231-263, doi:10.1007/BF00751331, (1995). 2) Malaspina, D.M., M. Horanyi, A. Zaslavsky, K. Goetz, L.B. Wilson III, and K. Kersten `Interplanetary and interstellar dust observed by the Wind/WAVES electric field instrument,` Geophys. Res. Lett. Vol. 41, pp. 266-272, doi:10.1002/2013GL058786, (2014). 3) Malaspina, D.M., and L.B. Wilson III `A Database of Interplanetary and Interstellar Dust Detected by the Wind Spacecraft, J. Geophys. Res., doi:10.1002/2016JA023209, (2016).
- Data Variable Descriptions
- Peak amplitude (mV) on Ch 1 [Ch01___Peak_amplitude]
The peak amplitude of the electric field component from the dust impact. This is the peak amplitude measured during a TDSF event on both antenna. This is a signed (i.e., +/-) value. The X-antenna was first cut on August 3, 2000. It was cut again on September 24, 2002. Currently, the effective antenna lengths used are 41.1 m, 3.79 m, and 2.17 m for the X-, Y-, and Z-antenna, respectively, for all dust impacts. We have removed these antenna length dependencies, which is why the amplitude units are in mV.
- Value of cross-correlation on Ch 1 [Ch01___cc_value]
The cross-correlation value between Ch 1 waveform and the normalized median waveform of a given morphological type [e.g., see Malaspina and Wilson, (2016) for morphological type definitions].
- Threshold value allowed for cross-correlation on Ch 1 [Ch01___cc_threshold]
The cross-correlation threshold value for the Ch 1 waveform used. The overall cross-correlation threshold is 0.8 but morphological types C, D, and M are required to exceed 0.9.
- Event selection threshold amplitude (mV) on Ch 1 [MinCh1_threshold]
The minimum Ch 1 absolute amplitude required for event selection. The X-antenna was first cut on August 3, 2000. It was cut again on September 24, 2002. Currently, the effective antenna lengths used are 41.1 m, 3.79 m, and 2.17 m for the X-, Y-, and Z-antenna, respectively, for all dust impacts. We have removed these antenna length dependencies, which is why the amplitude units are in mV.
- Avg. clockwise angle (degrees) of closest Ex antenna (to dust impact on spacecraft bus) from Earth-sun line (i.e., roughly +X-GSE) [Ch1ImpAnt_E_S_Angle]
The angle accounts for the XY-GSE displacement of Wind but assumes Earth remains at exactly 1 AU always. The error introduced by not including the change of the Earth's radial position throughout its annual orbit is less than ~0.017 degrees. The error introduced by not including the change of the spacecraft's out-of-ecliptic displacement is less than ~0.0018 degrees. The spacecraft (SC) spin axis is aligned within ~0.8 degrees of the south ecliptic pole. This varies annually due to the differences in torque applied to the SC bus by solar radiation. The angle can be as low as < 0.1 degrees.We define clockwise (CW) angles as being < 0 for CW rotations to remain consistent with Euler angle notation. We define CW as viewed from the north ecliptic pole looking down upon the XY-GSE plane. All angles herein vary from 0 to 360 degrees (absolute values), thus a positive counter-clockwise angle corresponds to [(clockwise angle) + 360] > 0. The impact antenna angle depends upon the closest impact antenna, defined by the CDF variables Ch01___ImpactAntenna and Ch02___ImpactAntenna. An example image illustrating the various angles within these CDF files can be found in the Malaspina and Wilson, [2016] (doi:10.1002/2016JA023209)
- Peak amplitude (mV) on Ch 2 [Ch02___Peak_amplitude]
The peak amplitude of the electric field component from the dust impact. This is the peak amplitude measured during a TDSF event on both antenna. This is a signed (i.e., +/-) value. The X-antenna was first cut on August 3, 2000. It was cut again on September 24, 2002. Currently, the effective antenna lengths used are 41.1 m, 3.79 m, and 2.17 m for the X-, Y-, and Z-antenna, respectively, for all dust impacts. We have removed these antenna length dependencies, which is why the amplitude units are in mV.
- Value of cross-correlation on Ch 2 [Ch02___cc_value]
The cross-correlation value between Ey waveform and the normalized median waveform of a given morphological type.
- Threshold value allowed for cross-correlation on Ch 2 [Ch02___cc_threshold]
The cross-correlation threshold value for the Ch 2 waveform used.
- Event selection threshold amplitude (mV) on Ch 2 [MinCh2_threshold]
The minimum Ch 2 absolute amplitude required for event selection. The X-antenna was first cut on August 3, 2000. It was cut again on September 24, 2002. Currently, the effective antenna lengths used are 41.1 m, 3.79 m, and 2.17 m for the X-, Y-, and Z-antenna, respectively, for all dust impacts. We have removed these antenna length dependencies, which is why the amplitude units are in mV.
- Avg. clockwise angle (degrees) of closest Ey antenna (to dust impact on spacecraft bus) from Earth-sun line (i.e., roughly +X-GSE) [Ch2ImpAnt_E_S_Angle]
The angle accounts for the XY-GSE displacement of Wind but assumes Earth remains at exactly 1 AU always. The error introduced by not including the change of the Earth's radial position throughout its annual orbit is less than ~0.017 degrees. The error introduced by not including the change of the spacecraft's out-of-ecliptic displacement is less than ~0.0018 degrees. The spacecraft (SC) spin axis is aligned within ~0.8 degrees of the south ecliptic pole. This varies annually due to the differences in torque applied to the SC bus by solar radiation. The angle can be as low as < 0.1 degrees.We define clockwise (CW) angles as being < 0 for CW rotations to remain consistent with Euler angle notation. We define CW as viewed from the north ecliptic pole looking down upon the XY-GSE plane. All angles herein vary from 0 to 360 degrees (absolute values), thus a positive counter-clockwise angle corresponds to [(clockwise angle) + 360] > 0. The impact antenna angle depends upon the closest impact antenna, defined by the CDF variables Ch01___ImpactAntenna and Ch02___ImpactAntenna. An example image illustrating the various angles within these CDF files can be found in the Malaspina and Wilson, [2016] (doi:10.1002/2016JA023209)
- Avg. clockwise angle (degrees) of +Ex antenna from spacecraft-sun line [Pos_Ax_SCS_Angle]
The angle accounts for the XY-GSE displacement of Wind but assumes Earth remains at exactly 1 AU always. The error introduced by not including the change of the Earth's radial position throughout its annual orbit is less than ~0.017 degrees. The error introduced by not including the change of the spacecraft's out-of-ecliptic displacement is less than ~0.0018 degrees. The spacecraft (SC) spin axis is aligned within ~0.8 degrees of the south ecliptic pole. This varies annually due to the differences in torque applied to the SC bus by solar radiation. The angle can be as low as < 0.1 degrees.We define clockwise (CW) angles as being < 0 for CW rotations to remain consistent with Euler angle notation. We define CW as viewed from the north ecliptic pole looking down upon the XY-GSE plane. All angles herein vary from 0 to 360 degrees (absolute values), thus a positive counter-clockwise angle corresponds to [(clockwise angle) + 360] > 0. The impact antenna angle depends upon the closest impact antenna, defined by the CDF variables Ch01___ImpactAntenna and Ch02___ImpactAntenna. An example image illustrating the various angles within these CDF files can be found in the Malaspina and Wilson, [2016] (doi:10.1002/2016JA023209)
- Avg. clockwise angle (degrees) of +Ex antenna from Earth-sun line (i.e., roughly +X-GSE) [Pos_Ax_E_S_Angle]
The angle accounts for the XY-GSE displacement of Wind but assumes Earth remains at exactly 1 AU always. The error introduced by not including the change of the Earth's radial position throughout its annual orbit is less than ~0.017 degrees. The error introduced by not including the change of the spacecraft's out-of-ecliptic displacement is less than ~0.0018 degrees. The spacecraft (SC) spin axis is aligned within ~0.8 degrees of the south ecliptic pole. This varies annually due to the differences in torque applied to the SC bus by solar radiation. The angle can be as low as < 0.1 degrees.We define clockwise (CW) angles as being < 0 for CW rotations to remain consistent with Euler angle notation. We define CW as viewed from the north ecliptic pole looking down upon the XY-GSE plane. All angles herein vary from 0 to 360 degrees (absolute values), thus a positive counter-clockwise angle corresponds to [(clockwise angle) + 360] > 0. The impact antenna angle depends upon the closest impact antenna, defined by the CDF variables Ch01___ImpactAntenna and Ch02___ImpactAntenna. An example image illustrating the various angles within these CDF files can be found in the Malaspina and Wilson, [2016] (doi:10.1002/2016JA023209)
- Avg. clockwise angle (degrees) of +Ey antenna from Earth-sun line (i.e., roughly +X-GSE) [Pos_Ay_E_S_Angle]
The angle accounts for the XY-GSE displacement of Wind but assumes Earth remains at exactly 1 AU always. The error introduced by not including the change of the Earth's radial position throughout its annual orbit is less than ~0.017 degrees. The error introduced by not including the change of the spacecraft's out-of-ecliptic displacement is less than ~0.0018 degrees. The spacecraft (SC) spin axis is aligned within ~0.8 degrees of the south ecliptic pole. This varies annually due to the differences in torque applied to the SC bus by solar radiation. The angle can be as low as < 0.1 degrees.We define clockwise (CW) angles as being < 0 for CW rotations to remain consistent with Euler angle notation. We define CW as viewed from the north ecliptic pole looking down upon the XY-GSE plane. All angles herein vary from 0 to 360 degrees (absolute values), thus a positive counter-clockwise angle corresponds to [(clockwise angle) + 360] > 0. The impact antenna angle depends upon the closest impact antenna, defined by the CDF variables Ch01___ImpactAntenna and Ch02___ImpactAntenna. An example image illustrating the various angles within these CDF files can be found in the Malaspina and Wilson, [2016] (doi:10.1002/2016JA023209)
- Uncertainty in Pos_Ax_E_S_Angle [Pos_Ax_E_S_Delta_Angle]
The angle accounts for the XY-GSE displacement of Wind but assumes Earth remains at exactly 1 AU always. The error introduced by not including the change of the Earth's radial position throughout its annual orbit is less than ~0.017 degrees. The error introduced by not including the change of the spacecraft's out-of-ecliptic displacement is less than ~0.0018 degrees. The spacecraft (SC) spin axis is aligned within ~0.8 degrees of the south ecliptic pole. This varies annually due to the differences in torque applied to the SC bus by solar radiation. The angle can be as low as < 0.1 degrees.We define clockwise (CW) angles as being < 0 for CW rotations to remain consistent with Euler angle notation. We define CW as viewed from the north ecliptic pole looking down upon the XY-GSE plane. All angles herein vary from 0 to 360 degrees (absolute values), thus a positive counter-clockwise angle corresponds to [(clockwise angle) + 360] > 0. The impact antenna angle depends upon the closest impact antenna, defined by the CDF variables Ch01___ImpactAntenna and Ch02___ImpactAntenna. An example image illustrating the various angles within these CDF files can be found in the Malaspina and Wilson, [2016] (doi:10.1002/2016JA023209)
- Uncertainty in E[x,y]_ImpAnt_E_S_Angle [ImpAnt_E_S_Delta_Angle]
The impact angle uncertainties are mostly controlled by the quadrant or hemisphere in which the dust impact occurred. This is true for the Ch1ImpAnt_E_S_Angle and Ch2ImpAnt_E_S_Angle. This is roughly +/- 45 degrees (i.e., quadrant) for all events. For the other sun angles (i.e., Pos_Ax_SCS_Angle, Pos_Ax_E_S_Angle, and Pos_Ay_E_S_Angle), the uncertainty is controlled by the spin rate of the spacecraft (determined by event duration and angle subtended during an event) multiplied by the TDSF event duration plus the DPU clock latency uncertainty (i.e., ~10.6 ms). Thus, this uncertainty is currently < 13 degrees (i.e., worst case scenario for fastest spin rate and slowest sampling rate). In the best case scenario (i.e., most events), the uncertainties drop to ~3 degrees.
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- WI_M0_SWE doi:10.48322/jsqc-vm88
- Description
Explanatory notes: The electron pitch-angle distribution averages included in this data set are derived from integrating the electron pitch-angle distributions measured by the Wind/SWE electron instrument (see Ogilvie et al., "SWE, a comprehensive plasma instrument for the Wind spacecraft", Space Sci. Rev., 71, 55, 1955). Averages of phase-space density (f) over key regions of the unit sphere (the set of all possible electron velocity directions) are computed from 9s measurements which are usually separated by one or more 3s spin-periods. These quantities are reliable and citable with caution, meaning that the PI advises that the user should discuss their interpretations with a member of the SWE science team before publishing. The following comments are intended to aid in the use and interpretation of the averages reported in this data set. We begin this analysis with a measure of f for each pitch-angle bin, six degrees in width, from 0 degrees (flux nearly parallel to B) to 180 degrees (flux nearly anti-parallel with B). The f values for pitch-angles from 0-90 degrees (parallel streaming) are integrated (with angluar weighting and assumptions of gyrotropy) over this half-sphere, then averaged by dividing out the 2-pi solid angle of the half-sphere; the result being referred to as the 'f_para' average. Similarly, the 'f_perp' (flux nearly perpendicular to B) average is the result of integrating f for pitch-angles from 60-120 degrees (a region also 2-pi in solid angle). Next, the 'f_anti' (flux nearly anti-parallel to B) average covers the half-sphere of "backward" streaming electrons; having pitch-angles from 90-180 degrees. Finally, the 'f_omni' (omni-directional) average provides the integral of f over the full sphere, divided by the full 4-pi solid angle; providing a measure of total electron flux into the region of observation. The above analysis is carried out for each of 13 energy channels: E = 19.34, 38.68, 58.03, 77.37, 96.71, 116.1, 193.4, 290.1, 425.5, 580.3, 773.7, 1006., and 1238. eV. For reference, the electron speeds (|V|, in cm/s) corresponding to these energies are reported in this data set. Hence the data set reported here contains: f_para, f_perp, f_anti, f_omni (for each of 13 values of E), and the 13 values of |V| (constant, included for reference).
- Modification History
Skeleton created 5/25/2007
- Data Variable Descriptions
- Electron flux, parallel average [f_para]
For each flux value, f_para[i], Ve[i] gives the corresponding electron speed (cm/s).
- --> stack plot for all channels, by speed [f_para_all]
For each flux value, f_para[i], Ve[i] gives the corresponding electron speed (cm/s).
- --> stack plot for even channels, by speed [f_para_even]
For each flux value, f_para[i], Ve[i] gives the corresponding electron speed (cm/s).
- --> stack plot for odd channels, by speed [f_para_odd]
For each flux value, f_para[i], Ve[i] gives the corresponding electron speed (cm/s).
- --> stack plot for all channels, by energy [f_para_all_2]
For each flux value, f_para[i], Ve[i] gives the corresponding electron speed (cm/s).
- --> stack plot for even channels, by energy [f_para_even_2]
For each flux value, f_para[i], Ve[i] gives the corresponding electron speed (cm/s).
- --> stack plot for odd channels, by energy [f_para_odd_2]
For each flux value, f_para[i], Ve[i] gives the corresponding electron speed (cm/s).
- Electron flux, perpendicular average [f_perp]
For each flux value, f_perp[i], Ve[i] gives the corresponding electron speed (cm/s).
- --> stack plot for all channels, by speed [f_perp_all]
For each flux value, f_perp[i], Ve[i] gives the corresponding electron speed (cm/s).
- --> stack plot for even channels, by speed [f_perp_even]
For each flux value, f_perp[i], Ve[i] gives the corresponding electron speed (cm/s).
- --> stack plot for odd channels, by speed [f_perp_odd]
For each flux value, f_perp[i], Ve[i] gives the corresponding electron speed (cm/s).
- --> stack plot for all channels, by energy [f_perp_all_2]
For each flux value, f_perp[i], Ve[i] gives the corresponding electron speed (cm/s).
- --> stack plot for even channels, by energy [f_perp_even_2]
For each flux value, f_perp[i], Ve[i] gives the corresponding electron speed (cm/s).
- --> stack plot for odd channels, by energy [f_perp_odd_2]
For each flux value, f_perp[i], Ve[i] gives the corresponding electron speed (cm/s).
- Electron flux, anti-parallel average [f_anti]
For each flux value, f_anti[i], Ve[i] gives the corresponding electron speed (cm/s).
- --> stack plot for all channels, by speed [f_anti_all]
For each flux value, f_anti[i], Ve[i] gives the corresponding electron speed (cm/s).
- --> stack plot for even channels, by speed [f_anti_even]
For each flux value, f_anti[i], Ve[i] gives the corresponding electron speed (cm/s).
- --> stack plot for odd channels, by speed [f_anti_odd]
For each flux value, f_anti[i], Ve[i] gives the corresponding electron speed (cm/s).
- --> stack plot for all channels, by energy [f_anti_all_2]
For each flux value, f_anti[i], Ve[i] gives the corresponding electron speed (cm/s).
- --> stack plot for even channels, by energy [f_anti_even_2]
For each flux value, f_anti[i], Ve[i] gives the corresponding electron speed (cm/s).
- --> stack plot for odd channels, by energy [f_anti_odd_2]
For each flux value, f_anti[i], Ve[i] gives the corresponding electron speed (cm/s).
- Electron flux, omni-directional average [f_omni]
For each flux value, f_omni[i], Ve[i] gives the corresponding electron speed (cm/s).
- --> stack plot for all channels, by speed [f_omni_all]
For each flux value, f_omni[i], Ve[i] gives the corresponding electron speed (cm/s).
- --> stack plot for even channels, by speed [f_omni_even]
For each flux value, f_omni[i], Ve[i] gives the corresponding electron speed (cm/s).
- --> stack plot for odd channels, by speed [f_omni_odd]
For each flux value, f_omni[i], Ve[i] gives the corresponding electron speed (cm/s).
- --> stack plot for all channels, by energy [f_omni_all_2]
For each flux value, f_omni[i], Ve[i] gives the corresponding electron speed (cm/s).
- --> stack plot for even channels, by energy [f_omni_even_2]
For each flux value, f_omni[i], Ve[i] gives the corresponding electron speed (cm/s).
- --> stack plot for odd channels, by energy [f_omni_odd_2]
For each flux value, f_omni[i], Ve[i] gives the corresponding electron speed (cm/s).
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- WI_M2_SWE doi:10.48322/dq7x-fd74
- Description
Explanatory notes: The electron pitch-angle distribution averages included in this data set are derived from integrating the electron pitch-angle distributions measured by the Wind/SWE electron instrument (see Ogilvie et al., "SWE, a comprehensive plasma instrument for the Wind spacecraft", Space Sci. Rev., 71, 55, 1955). Averages of phase-space density (f) over key regions of the unit sphere (the set of all possible electron velocity directions) are computed from 3s measurements which are spaced either 6s or 12s in time. These quantities are reliable and citable with caution, meaning that the PI advises that the user should discuss their interpretations with a member of the SWE science team before publishing. The following comments are intended to aid in the use and interpretation of the averages reported in this data set. We begin this analysis with a measure of f for each pitch-angle bin, six degrees in width, from 0 degrees (flux nearly parallel to B) to 180 degrees (flux nearly anti-parallel with B). The f values for pitch-angles from 0-90 degrees (parallel streaming) are integrated (with angluar weighting and assumptions of gyrotropy) over this half-sphere, then averaged by dividing out the 2-pi solid angle of the half-sphere; the result being referred to as the 'f_para' average. Similarly, the 'f_perp' (flux nearly perpendicular to B) average is the result of integrating f for pitch-angles from 60-120 degrees (a region also 2-pi in solid angle). Next, the 'f_anti' (flux nearly anti-parallel to B) average covers the half-sphere of "backward" streaming electrons; having pitch-angles from 90-180 degrees. Finally, the 'f_omni' (omni-directional) average provides the integral of f over the full sphere, divided by the full 4-pi solid angle; providing a measure of total electron flux into the region of observation. The above analysis is carried out for each of 16 energy channels ranging from about 10 eV to as much as 3 keV. The exact energies at which observations are made is time-varying, and this data set reports the electron speeds each channel observes (|V|, in cm/s, along with the observations themselves) at any time. Hence the data set reported here contains: f_para, f_perp, f_anti, f_omni (for each of 16 values of |V|), and the 16 values of |V| (time-varying, although usually much more slowly than the order of a day).
- Modification History
Skeleton created 12/17/2007
- Data Variable Descriptions
- Electron speed [Ve]
time-varying electron speeds corresponding to fluxes
- --> Stack plot of Electron speed [Ve_stack]
time-varying electron speeds corresponding to fluxes
- Electron energy [eV]
electron speeds corresponding to fluxes
- --> Stack plot of Electron energy [eV_stack]
electron speeds corresponding to fluxes
- Electron flux, parallel average [f_para]
For each flux value, f_para[i], Ve[i] gives the corresponding electron speed (cm/s).
- --> stack plot for all channels [f_para_all]
For each flux value, f_para[i], Ve[i] gives the corresponding electron speed (cm/s).
- --> stack plot for even channels [f_para_even]
For each flux value, f_para[i], Ve[i] gives the corresponding electron speed (cm/s).
- --> stack plot for odd channels [f_para_odd]
For each flux value, f_para[i], Ve[i] gives the corresponding electron speed (cm/s).
- Electron flux, perpendicular average [f_perp]
For each flux value, f_perp[i], Ve[i] gives the corresponding electron speed (cm/s).
- --> stack plot for all channels [f_perp_all]
For each flux value, f_perp[i], Ve[i] gives the corresponding electron speed (cm/s).
- --> stack plot for even channels [f_perp_even]
For each flux value, f_perp[i], Ve[i] gives the corresponding electron speed (cm/s).
- --> stack plot for odd channels [f_perp_odd]
For each flux value, f_perp[i], Ve[i] gives the corresponding electron speed (cm/s).
- Electron flux, anti-parallel average [f_anti]
For each flux value, f_anti[i], Ve[i] gives the corresponding electron speed (cm/s).
- --> stack plot for all channels [f_anti_all]
For each flux value, f_anti[i], Ve[i] gives the corresponding electron speed (cm/s).
- --> stack plot for even channels [f_anti_even]
For each flux value, f_anti[i], Ve[i] gives the corresponding electron speed (cm/s).
- --> stack plot for odd channels [f_anti_odd]
For each flux value, f_anti[i], Ve[i] gives the corresponding electron speed (cm/s).
- Electron flux, omni-directional average [f_omni]
For each flux value, f_omni[i], Ve[i] gives the corresponding electron speed (cm/s).
- --> stack plot for all channels [f_omni_all]
For each flux value, f_omni[i], Ve[i] gives the corresponding electron speed (cm/s).
- --> stack plot for even channels [f_omni_even]
For each flux value, f_omni[i], Ve[i] gives the corresponding electron speed (cm/s).
- --> stack plot for odd channels [f_omni_odd]
For each flux value, f_omni[i], Ve[i] gives the corresponding electron speed (cm/s).
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- WI_OR_DEF doi:10.48322/t0jm-c908
- Description
TBS
- Modification History
Originated Monday, May 13, 1991 Modified June 13, 1991 for version 2.1 Modified October 2,1991 for new global attributes, incr sizes Modified 11/11/91 Add sun vector, replace space id with support id Modified 1992 Feb 11 to use the variable name TIME and type CDF_INT4 instead of EPOCH and CDF_EPOCH for the time tags CCR 490 Modified 6/2/92 add project, discipline, source_name, data_version, title, and mods to global section; add validmin, validmax, labl_ptr_1 and monoton attributes to some variables; put epoch time back in, rename time to time_pb5; add label_time to variables Modified 11/07/92 to use Epoch and Time_PB5 variable name Modified 6/2/93 add ADID_ref and Logical_file_id 7/5/94 - CCR ISTP 1852 updated CDHF skeleton to CDF standards - JT 9/21/94 - Added 24 new global attributes to log the ephemeris comparison summary report from the definitive FDF orbit file. CCR 1932 11/7/94 - Merged CCR 1852 changes and corrected errors made in CCR 1852. ICCR 1884 12/7/94 - Modified MODS to follow ISTP standards. ICCR 1885 01/05/95 - add heliocentric coordinate system. CCR 1889 2/28/95 - added COMMENT1 and COMMENT2 for CCR 11/03/95 - deleted crn_space for CCR 2154 - RM 09/20/96 - changed CRN to CRN_EARTH for CCR 2269
- Data Variable Descriptions
- J2000 GCI Cartesian Position [GCI_POS]
- J2000 GCI Cartesian Velocity [GCI_VEL]
- GSE Cartesian Position [GSE_POS]
- GSE Cartesian Velocity [GSE_VEL]
- GSM Cartesian Position [GSM_POS]
- GSM Cartesian Velocity [GSM_VEL]
- J2000 GCI Sun Position Vector [SUN_VECTOR]
- HEC Cartesian Position [available starting around 1995/05/01] [HEC_POS]
- HEC Cartesian Velocity [available starting around 1995/05/01] [HEC_VEL]
- Carrington Rotation Number [available starting after 1996/03/01] [CRN_EARTH]
- Heliographic Long of Earth [available starting around 1995/05/01] [LONG_EARTH]
- Heliographic Lat of Earth [available starting around 1995/05/01] [LAT_EARTH]
- Heliographic Long of Craft [available starting around 1995/05/01] [LONG_SPACE]
- Heliographic Lat of Craft [available starting around 1995/05/01] [LAT_SPACE]
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- Data Variable Descriptions
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- WI_OR_PRE doi:10.48322/73de-sf52
- Description
TBS
- Modification History
Originated Monday, May 13, 1991 Modified June 13, 1991 for version 2.1 Modified October 2,1991 for new global attributes, incr sizes Modified 11/11/91 Add sun vector, replace space id with support id Modified 1992 Feb 11 to use the variable name TIME and type CDF_INT4 instead of EPOCH and CDF_EPOCH for the time tags CCR 490 Modified 6/2/92 add project, discipline, source_name, data_version, title, and mods to global section; add validmin, validmax, labl_ptr_1 and monoton attributes to some variables; put epoch time back in, rename time to time_pb5; add label_time to variables Modified 11/07/92 to use Epoch and Time_PB5 variable name Modified 6/2/93 add ADID_ref and Logical_file_id 7/5/94 - CCR ISTP 1852 updated CDHF skeleton to CDF standards - JT 9/21/94 - Added 24 new global attributes to log the ephemeris comparison summary report from the definitive FDF orbit file. CCR 1932 11/7/94 - Merged CCR 1852 changes and corrected errors made in CCR 1852. ICCR 1884 12/7/94 - Modified MODS to follow ISTP standards. ICCR 1885 01/05/95 - add heliocentric coordinate system. CCR 1889 2/28/95 - added COMMENT1 and COMMENT2 for CCR 11/03/95 - deleted crn_space for CCR 2154 - RM 09/20/96 - changed CRN to CRN_EARTH for CCR 2269
- Data Variable Descriptions
- J2000 GCI Cartesian Position (orbit display) [GCI_POS]
- J2000 GCI Cartesian Position (time-series display) [GCI_POS_t]
- J2000 GCI Cartesian Velocity [GCI_VEL]
- GSE Cartesian Position (orbit display) [GSE_POS]
- GSE Cartesian Position (time-series display) [GSE_POS_t]
- GSE Cartesian Velocity [GSE_VEL]
- GSM Cartesian Position (orbit display) [GSM_POS]
- GSM Cartesian Position (time-series display) [GSM_POS_t]
- GSM Cartesian Velocity [GSM_VEL]
- J2000 GCI Sun Position Vector [SUN_VECTOR]
- HEC Cartesian Position (orbit display, available after 1995/05/10) [HEC_POS]
- HEC Cartesian Position (time-series display, available after 1995/05/10) [HEC_POS_t]
- HEC Cartesian Velocity [HEC_VEL]
- Carrington Rotation Number (available from 1995/05/10 - 1996/03/19 and 1996/11/20 on) [CRN_EARTH]
- Heliographic Long of Earth (available from 1995/05/10) [LONG_EARTH]
- Heliographic Lat of Earth (available from 1995/05/10) [LAT_EARTH]
- Heliographic Long of Craft (available from 1995/05/10) [LONG_SPACE]
- Heliographic Lat of Craft (available from 1995/05/10) [LAT_SPACE]
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- WI_PLSP_3DP doi:10.48322/c4mf-9n52
- Description
Wind 3dp, PESA Low (~24 sec resolution) energy spectra with ion moments
- Data Variable Descriptions
- [FLUX] Proton number flux, 15 energy channels populated approximately 0.4-3 keV [spectrogram] [FLUX]
Proton number flux in 14 energy channels populated from about 0.6 keV to about 10 keV. Channel energies vary with time, keeping the peak flux in channel 10. Channel 15 is the lowest energy channel.
- ---> As stacked plot [FLUX_STACKED]
- ---> Time-variable energy in each of 15 channels [ENERGY]
Energy, for 14 channels ~0.6 to ~10 KeV
- [P.SC_CURRENT?] Current contribution to the spacecraft from thermal protons [MOM.P.SC_CURRENT]
- ---> [P.MAGF] magnetic field vector interpolated (linearly) to the time of the PESA Low distribution, in GSE cartesian components [MOM.P.MAGF]
- ---> [P.DENSITY] Proton number density [MOM.P.DENSITY]
- ---> [P.AVGTEMP] Average proton temperature [MOM.P.AVGTEMP]
- ---> [P.VTHERMAL] Proton most probable speed [MOM.P.VTHERMAL]
- ---> [P.VELOCITY] Proton Flow Velocity, GSE cartesian [MOM.P.VELOCITY]
- ---> [P.FLUX] Proton total number flux - cartesian GSE [MOM.P.FLUX]
- [P.PTENS] Proton Pressure Tensor calculated in the GSE coordinate basis. The elements correspond to, in the following order: XX, YY, ZZ, XY, XZ, YZ [MOM.P.PTENS]
- ---> [P.MFTENS] Proton Momentum Flux Tensor calculated in the GSE coordinate basis. The elements correspond to, in the following order: XX, YY, ZZ, XY, XZ, YZ [MOM.P.MFTENS]
- ---> [P.EFLUX] Proton eflux [MOM.P.EFLUX]
- ---> [P.T3] Proton Temperature eigenvalues after diagonalization of tensor, calculated in the GSE coordinate basis. The elements correspond to: XX, YY, ZZ [MOM.P.T3]
- [P.SYMM] Symmetry direction of proton pressure tensor, calculated in the GSE coordinate basis. The elements correspond to: XX, YY, ZZ and are defined by the largest eigenvalue in .T3 [MOM.P.SYMM]
- ---> [P.SYMM_THETA] Proton symmetry direction, latitude [MOM.P.SYMM_THETA]
- ---> [P.SYMM_PHI] Proton symmetry direction, longitude [MOM.P.SYMM_PHI]
- ---> [P.SYMM_ANG] Angle between proton symmetry direction and the magnetic field vector [MOM.P.SYMM_ANG]
- ---> [P.SYMM_MAGT3] Proton temperature tensor... rotated into a field-aligned coordinate basis and then taking the diagonal elements only [MOM.P.MAGT3]
The elements then correspond to: Perp_1, Perp_2, Parallel (with respect to .MAGF). Let V = .VELOCITY, B = .MAGF, then: Perp_1 = (B x V) x B, Perp_2 = (B x V) and Then T_perp = (MAGT3[0] + MAGT3[1])/2.
- [P.ERANGE] Proton energy range used to compute the moments [MOM.P.ERANGE]
- ---> [P.MASS] Proton mass of species [MOM.P.MASS]
- ---> [P.VALID] Proton Validity flag; 1=OK [MOM.P.VALID]
- [P.VEL_MAG] Proton flow speed [MOM.P.VEL_MAG]
- ---> [P.VEL_TH] Proton flow velocity; latitude/theta [MOM.P.VEL_TH]
- ---> [P.VELPHI] Proton flow velocity; longitude/phi [MOM.P.VEL_PHI]
- [A.SC_CURRENT] Current contribution to the spacecraft from thermal alphas [MOM.A.SC_CURRENT]
- ---> [A.MAGF] magnetic field vector interpolated (linearly) to the time of the PESA Low distribution, in GSE cartesian components [MOM.A.MAGF]
- ---> [A.DENSITY] Alpha number density [MOM.A.DENSITY]
- ---> [A.AVGTEMP] Average alpha temperature [MOM.A.AVGTEMP]
- ---> [A.VTHERMAL] Alpha most probable speed [MOM.A.VTHERMAL]
- ---> [A.VELOCITY] Alpha Flow Velocity, GSE cartesian [MOM.A.VELOCITY]
- ---> [P.FLUX] Alpha total number flux - cartesian GSE [MOM.A.FLUX]
- [A.PTENS] Alpha Pressure Tensor calculated in the GSE coordinate basis. The elements correspond to, in the following order: XX, YY, ZZ, XY, XZ, YZ [MOM.A.PTENS]
- ---> [A.MFTENS] Alpha Momentum Flux Tensor calculated in the GSE coordinate basis. The elements correspond to, in the following order: XX, YY, ZZ, XY, XZ, YZ [MOM.A.MFTENS]
- ---> [A.EFLUX] Alpha eflux [MOM.A.EFLUX]
- ---> [A.T3] Alpha Temperature eigenvalues after diagonalization of tensor, calculated in the GSE coordinate basis. The elements correspond to: XX, YY, ZZ [MOM.A.T3]
- [A.SYMM] Symmetry direction of alpha pressure tensor, calculated in the GSE coordinate basis. The elements correspond to: XX, YY, ZZ and are defined by the largest eigenvalue in .T3 [MOM.A.SYMM]
- ---> [A.SYMM_THETA] Alpha symmetry direction, latitude [MOM.A.SYMM_THETA]
- ---> [A.SYMM_PHI] Alpha symmetry direction, longitude [MOM.A.SYMM_PHI]
- ---> [A.SYMM_ANG] Angle between alpha symmetry direction and magnetic field vector [MOM.A.SYMM_ANG]
- ---> [A.SYMM_MAGT3] Alpha temperature tensor... rotated into a field-aligned coordinate basis and then taking the diagonal elements only [MOM.A.MAGT3]
The elements then correspond to: Perp_1, Perp_2, Parallel (with respect to .MAGF). Let V = .VELOCITY, B = .MAGF, then: Perp_1 = (B x V) x B, Perp_2 = (B x V) and Then T_perp = (MAGT3[0] + MAGT3[1])/2.
- [A.ERANGE] Alpha energy range used to compute the moments [MOM.A.ERANGE]
- ---> [A.MASS] Alpha mass of species [MOM.A.MASS]
- ---> [A.VALID] Alpha validity flag; 1=OK [MOM.A.VALID]
- [A.VEL_MAG] Alpha flow speed [MOM.A.VEL_MAG]
- ---> [A.VEL_TH] Alpha flow velocity, latitude [MOM.A.VEL_TH]
- ---> [A.VEL_PHI] Alpha flow velocity, longitude [MOM.A.VEL_PHI]
- UNIX time; seconds since January 1, 1970 [TIME]
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- WI_PM_3DP doi:10.48322/s8e6-aw08
- Description
Wind 3dp, PESA LOW 1 spin resolution ion (proton and alpha) moments (computed on spacecraft)
- Modification History
Version 3 Product, August 2005
- Data Variable Descriptions
- Proton number density [values fill-noisy 5/19/2009-5/11/2010; 3/8-5/15/2012] [P_DENS]
Proton number density values are fill for time period 5/20/2009-5/11/2010; noisy 3/8/2012 04:37 to 5/15/2012 22:45]
- ---> Proton velocity vector (GSE) [P_VELS]
Proton velocity vector values are noisy for time period 5/15/2009-5/11/2010 and 3/8/2012 04:37 to 5/15/2012 22:45
- ---> Residual Variance in Proton Velocity (6 components in instrument coords) [P_TENS]
Residual Variance in Proton Velocity values are noisy for time period 5/15/2009-5/11/2010 and 3/8/2012 04:37 to 5/15/2012 22:45
- ---> Proton temperature [P_TEMP]
Proton temperature values are noisy for time period 5/15/2009-5/11/2010 and 3/8/2012 04:37 to 5/15/2012 22:45
- Alpha number density [values fill-noisy 5/19/2009-5/11/2010; 3/8-5/15/2012] [A_DENS]
Alpha number density values are fill for time period 5/15/2009-5/11/2010; noisy 3/8/2012 04:37 to 5/15/2012 22:45
- ---> Alpha velocity vector (GSE) [A_VELS]
Alpha velocity vector values are noisy for time period 5/15/2009-5/11/2010 and 3/8/2012 04:37 to 5/15/2012 22:45
- ---> Residual Variance in Alpha Velocity (6 components in instrument coords) [A_TENS]
Residual Variance in Alpha Velocity values are noisy for time period 5/15/2009-5/11/2010 and 3/8/2012 04:37 to 5/15/2012 22:45
- ---> Alpha temperature [A_TEMP]
Alpha temperature values are noisy for time period 5/15/2009-5/11/2010 and 3/8/2012 04:37 to 5/15/2012 22:45
- Energy range of moments computation [E_RANGE]
- Gap flag (0=no gap, 1=gap) [GAP]
- Data quality flag (1=good, 0=bad) [VALID]
- Unix Time (since 1970/01/01) [TIME]
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- WI_SFPD_3DP doi:10.48322/aawb-c884
- Description
Wind 3dp, SST Foil energetic electron pitch angle distributions. General Notes per Lynn Wilson Jan 2015: The solid-state telescope (SST) for Wind 3DP electrons returns a velocity distribution function containing 7 energy bins and 48 solid-angle bins. The automated CDF routine appears to remove all the following solid-angle bins: [7,8,9,15,31,32,33] = sun/anti-sun look directions, and [20,21,22,23,44,45,46,47] = low geometry factor bins (also correspond to the SST Thick anti-coincidence detector bins). The sun/anti-sun directions are removed to avoid X-ray and EUV contamination, which is often seen during solar flares. The onset looks exactly like the GOES X-ray observations, which is kind of fun but not what we want to look at. Unfortunately, these look directions can correspond to the magnetic field direction, which can limit the times when we would like to examine SEP events. General Notes per Lynn Wilson Jan 2015: Note that SST Open (e.g., wi_sopd_3dp_00000000_v01.cdf) software removes the following additional solid-angle bins: [0,1,24,25] = noisy. Additionally, SST Open has 9 energy channels from ~70 keV to ~6.7 or 7.1 MeV, depending on the mode the instrument is in. It does not appear that the routine mk_sosp_cdf.pro removes any of these ...bad... look directions, so that should be noted as well. General Notes per Lynn Wilson Jan 2015: Inside the radiation belts, both Foil and Open saturate and suffer from penetrating particles. The instruments are not shielded, so they can only provide relative changes when in these regions. General Notes per Lynn Wilson Jan 2015: The data all look like they are in units of number flux or # cm-2 s-1 sr-1 eV-1.
- Data Variable Descriptions
- Electron number flux 27 keV to 520 keV in 7 energy and 8 pitch angle bins (as energy-angle displays) [FLUX]
- Electron number flux 27 keV to 520 keV at 8 pitch angles as spectrograms by energy [FLUX_byE_atA]
- Electron number flux 27 keV to 520 keV as a stack_plot of 7 energies at the Bin1 angle (often ~15 deg) [FLUX_byE_atA_stackPA0]
- ---> As a stack_plot at the Bin2 angle (often ~35 deg) [FLUX_byE_atA_stackPA1]
- ---> As a stack_plot at the Bin3 angle (often ~57 deg) [FLUX_byE_atA_stackPA2]
- ---> As a stack_plot at the Bin4 angle (often ~80 deg) [FLUX_byE_atA_stackPA3]
- ---> As a stack_plot at the Bin5 angle (often ~102 deg) [FLUX_byE_atA_stackPA4]
- ---> As a stack_plot at the Bin6 angle (often ~123 deg) [FLUX_byE_atA_stackPA5]
- ---> As a stack_plot at the Bin7 angle (often ~145 deg) [FLUX_byE_atA_stackPA6]
- ---> As a stack_plot at the Bin8 angle (often ~165 deg) [FLUX_byE_atA_stackPA7]
- Electron number flux 27 keV - 520 keV at 7 energies as spectrograms by pitch angle [FLUX_byA_atE]
- Electron number flux 27 keV to 520 keV as a stack plot of 8 pitch angles at the Ch1 energy (often ~27 keV) [FLUX_byA_atE_stackE0]
- ---> As a stack plot at the Ch2 energy (often ~40.5 keV) [FLUX_byA_atE_stackE1]
- ---> As a stack plot at the Ch3 energy (often ~86 keV) [FLUX_byA_atE_stackE2]
- ---> As a stack plot at the Ch4 energy (often ~110 keV) [FLUX_byA_atE_stackE3]
- ---> As a stack plot at the Ch5 energy (often ~180 keV) [FLUX_byA_atE_stackE4]
- ---> As a stack plot at the Ch6 energy (often ~310 keV) [FLUX_byA_atE_stackE5]
- ---> As a stack plot at the Ch7 energy (often ~520 keV) [FLUX_byA_atE_stackE6]
- Time-varying electron pitch angles for 8 angular bins [PANGLE]
- ---> Time-varying electron energies for 7 channels [ENERGY_filled]
Uses fix-sparse to fill in nan energy values
- [MAGF] Magnetic field cartesian GSE vector [MAGF]
- UNIX time; seconds since January 1, 1970 [TIME]
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- WI_SFSP_3DP doi:10.48322/wd3x-9a34
- Description
Wind 3dp, SST Foil energetic electron omni directional energy spectra General Notes per Lynn Wilson Jan 2015: The solid-state telescope (SST) for Wind 3DP electrons returns a velocity distribution function containing 7 energy bins and 48 solid-angle bins. The automated CDF routine appears to remove all the following solid-angle bins: [7,8,9,15,31,32,33] = sun/anti-sun look directions, and [20,21,22,23,44,45,46,47] = low geometry factor bins (also correspond to the SST Thick anti-coincidence detector bins). The sun/anti-sun directions are removed to avoid X-ray and EUV contamination, which is often seen during solar flares. The onset looks exactly like the GOES X-ray observations, which is kind of fun but not what we want to look at. Unfortunately, these look directions can correspond to the magnetic field direction, which can limit the times when we would like to examine SEP events. General Notes per Lynn Wilson Jan 2015: Note that SST Open (e.g., wi_sopd_3dp_00000000_v01.cdf) software removes the following additional solid-angle bins: [0,1,24,25] = noisy. Additionally, SST Open has 9 energy channels from ~70 keV to ~6.7 or 7.1 MeV, depending on the mode the instrument is in. It does not appear that the routine mk_sosp_cdf.pro removes any of these ...bad... look directions, so that should be noted as well. General Notes per Lynn Wilson Jan 2015: Inside the radiation belts, both Foil and Open saturate and suffer from penetrating particles. The instruments are not shielded, so they can only provide relative changes when in these regions. General Notes per Lynn Wilson Jan 2015: The data below all look like they are in units of number flux or # cm-2 s-1 sr-1 eV-1. I believe the CDAWeb units are correct for most of these.
- Data Variable Descriptions
- Electron number flux 27 keV - 520 keV as a function of energy in 7 channels (spectrogram) [FLUX]
- ---> As stacked plot [FLUX_STACKED]
- ---> As simple time series [FLUX_SIMPLE]
- ---> Time-varying electron energies in 7 channels [ENERGY_filled]
Uses fix-sparse to fill in nan energy values
- UNIX time; seconds since January 1, 1970 [TIME]
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- WI_SOPD_3DP doi:10.48322/yw1c-yf03
- Description
Wind 3dp, SOPD
- Data Variable Descriptions
- Proton number flux 70-6800 keV in 9 energy and 8 pitch angle bins (as energy-angle displays) [FLUX]
- Proton number flux at 8 pitch angles as spectrograms by energy [FLUX_byE_atA]
- Proton number flux as a stack_plot of 9 energies at the Bin1 angle (often ~15 deg) [FLUX_byE_atA_stackPA0]
- ---> As a stack_plot at the Bin2 angle (often ~35 deg) [FLUX_byE_atA_stackPA1]
- ---> As a stack_plot at the Bin3 angle (often ~57 deg) [FLUX_byE_atA_stackPA2]
- ---> As a stack_plot at the Bin4 angle (often ~80 deg) [FLUX_byE_atA_stackPA3]
- ---> As a stack_plot at the Bin5 angle (often ~102 deg) [FLUX_byE_atA_stackPA4]
- ---> As a stack_plot at the Bin6 angle (often ~123 deg) [FLUX_byE_atA_stackPA5]
- ---> As a stack_plot at the Bin7 angle (often ~145 deg) [FLUX_byE_atA_stackPA6]
- ---> As a stack_plot at the Bin8 angle (often ~165 deg) [FLUX_byE_atA_stackPA7]
- Proton number flux at 9 energies as spectrograms by pitch angle [FLUX_byA_atE]
- Proton number flux as a stack plot of 8 pitch angles at the Ch1 energy (often ~70 keV) [FLUX_byA_atE_stackE0]
- ---> As a stack plot at the Ch2 energy (often ~130 keV) [FLUX_byA_atE_stackE1]
- ---> As a stack plot at the Ch3 energy (often ~210 keV) [FLUX_byA_atE_stackE2]
- ---> As a stack plot at the Ch4 energy (often ~330 keV) [FLUX_byA_atE_stackE3]
- ---> As a stack plot at the Ch5 energy (often ~550 keV) [FLUX_byA_atE_stackE4]
- ---> As a stack plot at the Ch6 energy (often ~1.0 MeV) [FLUX_byA_atE_stackE5]
- ---> As a stack plot at the Ch7 energy (often ~2.1 MeV) [FLUX_byA_atE_stackE6]
- ---> As a stack plot at the Ch8 energy (often ~4.4 MeV) [FLUX_byA_atE_stackE7]
- ---> As a stack plot at the Ch9 energy (often ~6.8 MeV) [FLUX_byA_atE_stackE8]
- Time-varying proton pitch angles in 8 angular bins [PANGLE]
- ---> Time-varying proton energies in 9 channels [ENERGY_filled]
Uses fixed-sparse to fill in nan'd energies
- SW Velocity vector (from ions and ground-based processing) [VSW]
- Vector magnetic field [MAGF]
- UNIX time; seconds since January 1, 1970 [TIME]
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- WI_SOSP_3DP doi:10.48322/wkk0-y398
- Description
Wind 3dp, SST Open energetic Proton omni directional energy spectra General Notes per Lynn Wilson Jan 2015: The solid-state telescope (SST) for Wind 3DP electrons returns a velocity distribution function containing 7 energy bins and 48 solid-angle bins. The automated CDF routine appears to remove all the following solid-angle bins: [7,8,9,15,31,32,33] = sun/anti-sun look directions, and [20,21,22,23,44,45,46,47] = low geometry factor bins (also correspond to the SST Thick anti-coincidence detector bins). The sun/anti-sun directions are removed to avoid X-ray and EUV contamination, which is often seen during solar flares. The onset looks exactly like the GOES X-ray observations, which is kind of fun but not what we want to look at. Unfortunately, these look directions can correspond to the magnetic field direction, which can limit the times when we would like to examine SEP events. General Notes per Lynn Wilson Jan 2015: Note that SST Open (e.g., wi_sopd_3dp_00000000_v01.cdf) software removes the following additional solid-angle bins: [0,1,24,25] = noisy. Additionally, SST Open has 9 energy channels from ~70 keV to ~6.7 or 7.1 MeV, depending on the mode the instrument is in. It does not appear that the routine mk_sosp_cdf.pro removes any of these ...bad... look directions, so that should be noted as well. General Notes per Lynn Wilson Jan 2015: Inside the radiation belts, both Foil and Open saturate and suffer from penetrating particles. The instruments are not shielded, so they can only provide relative changes when in these regions. General Notes per Lynn Wilson Jan 2015: The data below all look like they are in units of number flux or # cm-2 s-1 sr-1 eV-1. I believe the CDAWeb units are correct for most of these.
- Data Variable Descriptions
- Proton number flux 70 keV - 6.8 MeV as a function of energy in 9 channels (spectrogram) [FLUX]
- ---> As a stacked plot [FLUX_STACKED]
- ---> As simple time series [FLUX_SIMPLE]
- ---> Time-varying proton energies in 9 channels [ENERGY_filled]
Uses fixed-sparse to fill in nan'd energies
- UNIX time; seconds since January 1, 1970 [TIME]
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- WI_STRAHL0_SWE doi:10.48322/4mxn-2e20
- Description
Explanatory notes: The 2D electron angular distributions included in this data set were measured by the Wind/SWE strahl detector (see Ogilvie et al., "SWE, a comprehensive plasma instrument for the Wind spacecraft", Space Sci. Rev., 71, 55, 1995). Each angular distribution was measured at a single electron energy. The energy was selected by applying a voltage between the electrostatic analyzer plates. The detector sampled 32 energies between 19 eV and 1238 eV, and during normal operation would sweep through these energies one at a time with approximately 12 second cadence. The instrument's 12 anodes are set in a vertical pattern in a plane that contains the spacecraft spin axis, spanning a field of view +/-28 degrees centered around the ecliptic (with uneven angular spacing between anodes). Wind's spin axis is set at a right angle with the ecliptic plane, allowing different azimuthal angles to be sampled as the spacecraft spins (3 sec spin period). These azimuthal bins have a fixed separation of 3.53 degrees. Each strahl (and antistrahl) distribution measured by the spacecraft consists of a 14x12 angular grid of electron counts, that was measured at a fixed energy during a single spacecraft spin. Counts are converted into physical units of f (v) (e.g., cm^-6s^3) in the standard fashion by accounting for the detector efficiency and geometric factor. The data set reported here contains: f_strahl, f_antistrahl, f_strahl_counts, f_antistrahl_counts, phi_strahl, phi_antistrahl, theta, energy.
- Modification History
Skeleton created 9/6/2017 by Konstantinos Horaites
- Data Variable Descriptions
- f_strahl intensities versus Phi and Theta angles in sweep energy order (log scaled animated gifs) [f_strahl]
2D angular electron distribution in physical units (#/{cc*(cm/s)^3}). Measured at fixed energy in a fraction of a single spacecraft spin. "f_strahl" corresponds with the anti-sunward, field-aligned portion of the distribution function, which likely exhibits a pronounced strahl signature.- ---> f_strahl (linear scaled) [f_strahl_lin]
2D angular electron distribution in physical units (#/{cc*(cm/s)^3}). Measured at fixed energy in a fraction of a single spacecraft spin. "f_strahl" corresponds with the anti-sunward, field-aligned portion of the distribution function, which likely exhibits a pronounced strahl signature.- f_antistrahl intensities versus Phi and Theta angles in sweep energy order (log scaled animated gifs) [f_antistrahl]
2D angular electron distribution in physical units (#/{cc*(cm/s)^3}). Measured at fixed energy in a fraction of a single spacecraft spin. "f_antistrahl" corresponds with the sunward, field-aligned portion of the distribution function, which sometimes exhibits a pronounced antistrahl signature.- ---> f_antistrahl (linear scaled) [f_antistrahl_lin]
2D angular electron distribution in physical units (#/{cc*(cm/s)^3}). Measured at fixed energy in a fraction of a single spacecraft spin. "f_antistrahl" corresponds with the sunward, field-aligned portion of the distribution function, which sometimes exhibits a pronounced antistrahl signature.- f_strahl_counts intensities versus Phi and Theta angles in sweep energy order (log scaled animated gifs) [f_strahl_counts]
2D angular electron distribution (detector counts). Measured at fixed energy in a fraction of a single spacecraft spin. "f_strahl" corresponds with the anti-sunward, field-aligned portion of the distribution function, which likely exhibits a pronounced strahl signature.
- ---> f_strahl_counts (linear scaled) [f_strahl_counts_lin]
2D angular electron distribution (detector counts). Measured at fixed energy in a fraction of a single spacecraft spin. "f_strahl" corresponds with the anti-sunward, field-aligned portion of the distribution function, which likely exhibits a pronounced strahl signature.
- f_antistrahl_counts intensities versus Phi and Theta angles in sweep energy order (log scaled animated gifs) [f_antistrahl_counts]
2D angular electron distribution (detector counts). Measured at fixed energy in a fraction of a single spacecraft spin. "f_antistrahl" corresponds with the sunward, field-aligned portion of the distribution function, which sometimes exhibits a pronounced antistrahl signature.
- ---> f_antistrahl_counts (linear scaled) [f_antistrahl_counts_lin]
2D angular electron distribution (detector counts). Measured at fixed energy in a fraction of a single spacecraft spin. "f_antistrahl" corresponds with the sunward, field-aligned portion of the distribution function, which sometimes exhibits a pronounced antistrahl signature.
- Phi (GSE) associated with unit vector pointing in electron velocity direction, for the strahl distribution. [phi_strahl]
phi_strahl corresponds with azimuthal directions (phi GSE) sampled during the measurement of f_strahl.
- Phi (GSE) associated with unit vector pointing in electron velocity direction, for the antistrahl distribution. [phi_antistrahl]
phi_antistrahl corresponds with azimuthal directions (phi GSE) sampled during the measurement of f_antistrahl.
- Theta (GSE) associated with unit vector pointing in electron velocity direction [theta]
The 12 anodes of the SWE strahl detector are arranged in a fixed pattern, with non-uniform spacing.
- energy (in eV) of the sampled electrons used to construct the f_strahl and f_antistrahl distributions [energy]
the strahl detector swept through 32 different energies, one at a time, with ~12 seconds between each energy step.
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- WI_SW-ION-DIST_SWE-FARADAY doi:10.48322/6vrg-6n41
- Description
This data set provides the Faraday Cup positive ion charge flux [picoAmperes] as a function of epoch, cup number, orientation angle, and bias grid potential. For each time point, a full spectrum is comprised of charge flux measurements at the two Faraday Cup sensors at 20 azimuth angles for each of 31 energy-per-charge windows (1240 data points per spectrum). Spectra are built up over approximately 92-second intervals. Th effective area of the Faraday Cup sensor as a function of incidence angle onto the cup is also provided.
- Data Variable Descriptions
- [CDAWEB PLOTS NOT SUPPORTED] The total charge flux (current) incident on the collector of cup 1, in picoAmperes (E/Q-azimuth display) [cup1_qflux]
The noise limit of this measurement is approximately 0.69 pA...Models of charge flow into the cup from oblique angles to the cup axis should account for projection of the aperture onto the collector. The calibrated effective area of the cup is given as a function of incidence angle in the lookup table.
- The total charge flux (current) incident on the collector of cup 1, in picoAmperes (E/Q-azimuth display) [data monotonically sorted based on dependencies] [cup1_qflux_reorder]
The noise limit of this measurement is approximately 0.69 pA...Models of charge flow into the cup from oblique angles to the cup axis should account for projection of the aperture onto the collector. The calibrated effective area of the cup is given as a function of incidence angle in the lookup table.
- ---> Spectrograms by azimuth at sample E/Q [data monotonically sorted based on dependencies] [cup1_qflux_E]
The noise limit of this measurement is approximately 0.69 pA...Models of charge flow into the cup from oblique angles to the cup axis should account for projection of the aperture onto the collector. The calibrated effective area of the cup is given as a function of incidence angle in the lookup table.
- ---> Spectrograms by E/Q at sample azimuths [data monotonically sorted based on dependencies] [cup1_qflux_A]
The noise limit of this measurement is approximately 0.69 pA...Models of charge flow into the cup from oblique angles to the cup axis should account for projection of the aperture onto the collector. The calibrated effective area of the cup is given as a function of incidence angle in the lookup table.
- [CDAWEB PLOTS NOT SUPPORTED] The total charge flux (current) incident on the collector of cup 2, in picoAmperes (E/Q-azimuth display) [cup2_qflux]
The noise limit of this measurement is approximately 0.69 pA...Models of charge flow into the cup from oblique angles to the cup axis should account for projection of the aperture onto the collector. The calibrated effective area of the cup is given as a function of incidence angle in the lookup table.
- The total charge flux (current) incident on the collector of cup 2, in picoAmperes (E/Q-azimuth display) [data monotonically sorted based on dependencies] [cup2_qflux_reorder]
The noise limit of this measurement is approximately 0.69 pA...Models of charge flow into the cup from oblique angles to the cup axis should account for projection of the aperture onto the collector. The calibrated effective area of the cup is given as a function of incidence angle in the lookup table.
- ---> Spectrograms by azimuth at sample E/Q [data monotonically sorted based on dependencies] [cup2_qflux_E]
The noise limit of this measurement is approximately 0.69 pA...Models of charge flow into the cup from oblique angles to the cup axis should account for projection of the aperture onto the collector. The calibrated effective area of the cup is given as a function of incidence angle in the lookup table.
- ---> Spectrograms by E/Q at sample azimuths [data monotonically sorted based on dependencies] [cup2_qflux_A]
The noise limit of this measurement is approximately 0.69 pA...Models of charge flow into the cup from oblique angles to the cup axis should account for projection of the aperture onto the collector. The calibrated effective area of the cup is given as a function of incidence angle in the lookup table.
- Azimuthal angle of the cup 1 normal. [cup1_azimuth]
The azimuthal angle for cup 1, in degrees. This is the angle formed by the ecliptic plane component of the cup normal and the XGSE unit vector. Positive angles correspond to deflection into the YGSE direction.
- Azimuthal angle of the cup 1 normal. [data monotonically sorted] [cup1_azimuth_reorder]
The azimuthal angle for cup 1, in degrees. This is the angle formed by the ecliptic plane component of the cup normal and the XGSE unit vector. Positive angles correspond to deflection into the YGSE direction.
- ---> The Energy-per-charge of admitted ions, i.e. the bias potential of cup 1 (in Volts). [cup1_EperQ]
For each potential window, the bias oscillates over a small range. This is the central value of the range.
- ---> The Energy-per-charge of admitted ions, i.e. the bias potential of cup 1 (in Volts). [data monotonically sorted] [cup1_EperQ_reorder]
For each potential window, the bias oscillates over a small range. This is the central value of the range.
- ---> Range of Energy-per-charge of admitted ions, i.e. the range of the bias potential of cup 1 (in Volts). [cup1_EperQ_DEL]
For each potential window, the bias oscillates over a small range. This is the width of the range.
- Azimuthal angle of the cup 2 normal. [cup2_azimuth]
The azimuthal angle for cup 2, in degrees. ed This is the angle formed by the ecliptic plane component of the cup normal and the XGSE unit vector. Positive angles correspond to deflection into the YGSE direction.
- Azimuthal angle of the cup 2 normal. [data monotonically sorted] [cup2_azimuth_reorder]
The azimuthal angle for cup 2, in degrees. ed This is the angle formed by the ecliptic plane component of the cup normal and the XGSE unit vector. Positive angles correspond to deflection into the YGSE direction.
- ---> The Energy-per-charge of admitted ions, i.e. the bias potential of cup 2 (in Volts). [cup2_EperQ]
For each potential window, the bias oscillates over a small range. This is the central value of the range.
- ---> The Energy-per-charge of admitted ions, i.e. the bias potential of cup 2veri (in Volts). [data monotonically sorted] [cup2_EperQ_reorder]
For each potential window, the bias oscillates over a small range. This is the central value of the range.
- ---> Range of Energy-per-charge of admitted ions, i.e. the range of the bias potential of cup 2 (in Volts). [cup2_EperQ_DEL]
For each potential window, the bias oscillates over a small range. This is the width of the range.
- Boolean signifying whether SWE is in peak-tracking mode [tracking]
0=not tracking.1=tracking..In TRACKING mode, the EperQ window with maximum current signal is identified and the EperQ scanning range is continuously adjusted such that the scan begins five windows below the peak (or at the minimum voltage).
- ---> Boolean signifying whether SWE is in full-scan mode [full_scan]
0=limited scan.1=full scan..In full scan mode, the EperQ scanning range is the full range of the instrument. In limited scan mode, the EperQ scanning range is smaller. Typically, limited scan mode is used in conjunction with tracking in order to best resolve the ion core distributions.
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-
WI_WA_RAD1_L3_DF doi:10.25935/hegh-1r24
Proper citations should include the "Accessed on date" in the form . - Description
This file contains goniopolarimetry analytical inversion dataset for Wind/Waves, assuming an unpolarized extended radio source (U=V=Q=0). Data are calibrated in W/m^2/Hz. Caveat: Level 3 df data are computed with the following assumptions : (i) incoming wave properties do not change during a spacecraft rotation (~3 seconds), (ii) radio sources are unpolarized (U=V=Q=0), (iii) Only receiver noise is substracted, (iv) radio sources have an uniform brightness distribution, (v) Z antennas are not tilted
- Modification History
V01: INITIAL RELEASE. CODED NOV 2020, X.BONNIN (LESIA, CNRS) V02: UPDATE GATTRS/ZVARS TO BE AS MUCH AS POSSIBLE CONSISTENT WITH STEREO/WAVES L3 CDF DATA. UPDATE FLUX CALIBRATION. CODED APRIL 2023, X.BONNIN (LESIA, CNRS)
- Data Variable Descriptions
- Stokes I parameter of the incoming wave [STOKES_I]
Absolute flux density (i.e., I Stokes parameter) of the incoming wave. Derived from direction-finding inversion.The receiver background is already removed.
- Wave vector colatitude [WAVE_COLATITUDE_SRF]
Colatitude angle of the wave vector in the Wind Spacecraft Reference reference (SRF)
- Wave vector azimuth [WAVE_AZIMUTH_SRF]
Azimuth angle of the wave vector in the Wind Spacecraft Reference Frame (SRF)
- Radio source angular size radius [SOURCE_SIZE]
Radio source angular size radius, assuming an uniform brightness distribution.
- Signal modulation rate [MODULATION_RATE]
Signal modulation rate
- Quality flag; 3=Good, 1=problems, 2=survey, 4=received special treatment [QUALITY_FLAG]
Flag to indicate the quality of the data. Possible values are: 0=Bad data. 1=Known problems. 2=Survey data. 3=Good for publication. 4=Data which has received special treatment.
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