
Hourly averaged definitive multispacecraft interplanetary parameters data OMNI Data Documentation: https://omniweb.gsfc.nasa.gov/html/ow_data.html Additional data access options available at SPDF's OMNIWeb Service: https://omniweb.gsfc.nasa.gov/ow.html COHOWebformatted OMNI_M merged magnetic field and plasma data http://cohoweb.gsfc.nasa.gov/ Recent OMNI 1HR Updates News: https://omniweb.gsfc.nasa.gov/html/ow_news.html
created August 2003; conversion to ISTP/IACG CDFs via SKTEditor Feb 2000 Time tags in CDAWeb version were modified in March 2005 to use the CDAWeb convention of having midaverage time tags rather than OMNI's original convention of startofaverage time tags.
Derived parameters are obtained from the following equations. Magnetosonic Mach number = V/Magnetosonic_speedMagnetosonic speed = [(sound speed)**2 + (Alfv speed)**2]**0.5The Alfven speed = 20. * B / N**0.5The sound speed = 0.12 * [T + 1.28*10**5]**0.5
Hourly averaged definitive multispacecraft interplanetary parameters data The Heliographic Inertial (HGI) coordinates are Suncentered and inertially fixed with respect to an Xaxis directed along the intersection line of the ecliptic and solar equatorial planes. The solar equator plane is inclined at 7.25 degrees from the ecliptic. This direction was towards ecliptic longitude of 74.367 degrees on 1 January 1900 at 1200 UT; because of precession of the celestial equator, this longitude increases by 1.4 degrees/century. The Z axis is directed perpendicular and northward from the solar equator, and the Yaxis completes the righthanded set. This system differs from the usual heliographic coordinates (e.g. Carrington longitudes) which are fixed in the frame of the rotating Sun. The RTN system is fixed at a spacecraft (or the planet). The R axis is directed radially away from the Sun, the T axis is the cross product of the solar rotation axis and the R axis, and the N axis is the cross product of the R and T axes. At zero heliographic latitude, when the spacecraft is in the solar equatorial plane, the N and solar rotation axes are parallel. Latitude and longitude angles of solar wind plasma flow are generally measured from the radius vector away from the Sun. In all cases, latitude angles are positive for northgoing flow. The flow longitude angles have been treated differently for the nearEarth data, i.e. the OMNI, and for the deep space data. The flow is positive for the nearEarth data when coming from the right side of the Sun as viewed from the Earth, i.e. flowing toward +Y from X GSE or opposite to the direction of planetary motion. On the other hand, the flow longitudes for the deep space spacecraft use the opposite sign convection, i.e. positive for flow in the +T direction in the RTN system.
created July 2007; conversion to ISTP/IACG CDFs via SKTEditor Feb 2000 Time tags in CDAWeb version were modified in March 2005 to use the CDAWeb convention of having midaverage time tags rather than OMNI's original convention of startofaverage time tags.
Dataset in CDAWeb
1minute averaged definitive multispacecraft interplanetary parameters data Additional information for all parameters are available from OMNI Data Documentation: https://omniweb.gsfc.nasa.gov/html/HROdocum.html Additional data access options available at SPDF's OMNIWeb Service: https://omniweb.gsfc.nasa.gov/ow_min.html Recent omni high resolution updates Release Notes: https://omniweb.gsfc.nasa.gov/html/hro_news.html
created November 2006; conversion to ISTP/IACG CDFs via SKTEditor Feb 2000 Time tags in CDAWeb version were modified in March 2005 to use the CDAWeb convention of having midaverage time tags rather than OMNI's original convention of startofaverage time tags.
Derived parameters are obtained from the following equations. Magnetosonic Mach number = V/Magnetosonic_speedMagnetosonic speed = [(sound speed)**2 + (Alfv speed)**2]**0.5The Alfven speed = 20. * B / N**0.5The sound speed = 0.12 * [T + 1.28*10**5]**0.5
Derived parameters are obtained from the following equations. Alfven Mach number = (V * Np**0.5) / 20 * B
Derived parameters are obtained from the following equations. Electric field = V(km/s) * Bz (nT; GSM) * 10**3
Derived parameters are obtained from the following equations. Flow pressure = (2*10**6)*Np*Vp**2 nPa (Np in cm**3, Vp in km/s, subscript p for proton)
The following spacecraft ID's are used: ACE 71, Geotail 60, IMP 8 50, Wind 51
The following spacecraft ID's are used: ACE 71, Geotail 60, IMP 8 50, Wind 51
The percent (0100) of the points contributing to the 1min magnetic field averages whose phase front normal (PFN) was interpolated because neither the MVAB0 nor Cross Product shift techniques yielded a PFN that satisfied its respective tests.
Derived parameters are obtained from the following equations. Plasma beta = [(T*4.16/10**5) + 5.34] * Np / B**2 (B in nT)
Note that standard deviations for the two vectors are given as the square roots of the sum of squares of the standard deviations in the component averages. The component averages are given in the records but not their individual standard deviations.
Note that standard deviations for the two vectors are given as the square roots of the sum of squares of the standard deviations in the component averages. The component averages are given in the records but not their individual standard deviations. There are no phase front normal standard deviations in the 5min records. This word has fill (99.99) for such records.
5minute averaged definitive multispacecraft interplanetary parameters data Additional information for all parameters are available from OMNI Data Documentation: https://omniweb.gsfc.nasa.gov/html/HROdocum.html Additional data access options available at SPDF's OMNIWeb Service: https://omniweb.gsfc.nasa.gov/ow_min.html Recent omni high resolution updates Release Notes: https://omniweb.gsfc.nasa.gov/html/hro_news.html
created November 2006; conversion to ISTP/IACG CDFs via SKTEditor Feb 2000 Time tags in CDAWeb version were modified in March 2005 to use the CDAWeb convention of having midaverage time tags rather than OMNI's original convention of startofaverage time tags.
Derived parameters are obtained from the following equations. Electric field = V(km/s) * Bz (nT; GSM) * 10**3
Derived parameters are obtained from the following equations. Magnetosonic Mach number = V/Magnetosonic_speedMagnetosonic speed = [(sound speed)**2 + (Alfv speed)**2]**0.5The Alfven speed = 20. * B / N**0.5The sound speed = 0.12 * [T + 1.28*10**5]**0.5
Derived parameters are obtained from the following equations. Alfven Mach number = (V * Np**0.5) / 20 * B
Derived parameters are obtained from the following equations. Flow pressure = (2*10**6)*Np*Vp**2 nPa (Np in cm**3, Vp in km/s, subscript p for proton)
The following spacecraft ID's are used: ACE 71, Geotail 60, IMP 8 50, Wind 51
The following spacecraft ID's are used: ACE 71, Geotail 60, IMP 8 50, Wind 51
The percent (0100) of the points contributing to the 1min magnetic field averages whose phase front normal (PFN) was interpolated because neither the MVAB0 nor Cross Product shift techniques yielded a PFN that satisfied its respective tests.
Derived parameters are obtained from the following equations. Plasma beta = [(T*4.16/10**5) + 5.34] * Np / B**2 (B in nT)
Note that standard deviations for the two vectors are given as the square roots of the sum of squares of the standard deviations in the component averages. The component averages are given in the records but not their individual standard deviations.