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342 results for “Solar Wind”
ACE Electron Proton Alpha Monitor (EPAM) LEFS60 MFSA, Solar Wind Frame, Sectored Z>1 Ion Fluxes, 17 min Averages
17-min-averaged sectored Z>1 ion fluxes from the MF Spectrum Analyzer of the ACE/EPAM LEFS60 instrument. All energies thresholds take into account the incident particle type, shielding, and inactive dead-layer of the solid state detector. All fluxes are background corrected and are in the solar wind rest frame.
ACE Electron Proton Alpha Monitor (EPAM) LEFS/LEMS MFSA, Solar Wind Frame, Spin-Averaged Electron Fluxes, Daily Averages
Daily-averaged electron fluxes from the MF Spectrum Analyzer of the ACE/EPAM instrument. All energies thresholds take into account the incident particle type, shielding, and inactive dead-layer of the solid state detector. All fluxes are background corrected and are in the solar wind rest frame.
ACE Electron Proton Alpha Monitor (EPAM) LEFS150 MFSA, Solar Wind Frame, Sectored Z>1 Ion Fluxes, Hourly Averages
Hourly-averaged sectored Z>1 ion fluxes from the MF Spectrum Analyzer of the ACE/EPAM LEFS150 instrument. All energies thresholds take into account the incident particle type, shielding, and inactive dead-layer of the solid state detector. All fluxes are background corrected and are in the solar wind rest frame.
STEREO-A In-Situ Measurements of Particles and CME Transients from the Magnetometer and the Plasma and Suprathermal Ion and Composition Instruments (IMPACT/MAG, PLASTIC) Solar Wind Plasma Data
STEREO-A In-situ Measurements of Particles and CME Transients, IMPACT, Magnetometer Instrument, MAG, Magnetic Field Vector and PLAsma and SupraThermal Ion Composition, PLASTIC, Solar Wind Parameter, Level 2, Data
APOLLO 12 ALSEP/SWS SOLAR WIND 28-SEC RESOLUTION TABLES V1.0
This data set contains daily tables of time ordered, 28-second-resolution plasma parameters, mainly of the solar wind, as observed on the Moon at the Apollo 12 ALSEP site by the Apollo 12 Solar Wind Spectrometer from 19 November 1969 through 25 March 1976.
Wind 3DP Solar Wind Plasma Corrected Electron Moments (EMFITS), 100 s Data
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, 71, 125-153, 1995. C. S. Salem et al., Precision Electron Measurements in the Solar Wind at 1 AU 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, 119, 647-657, doi:10.1002/2013JA019359, 2014.
ACE Electron Proton Alpha Monitor (EPAM) LEFS/LEMS MFSA, Solar Wind Frame, Spin-Averaged Proton Fluxes, Hourly Averages
Hourly-averaged proton fluxes from the MF Spectrum Analyzer of the ACE/EPAM instrument. All energies thresholds take into account the incident particle type, shielding, and inactive dead-layer of the solid state detector. All fluxes are background corrected and are in the solar wind rest frame.
ACE Electron Proton Alpha Monitor (EPAM) LEFS60 MFSA, Solar Wind Frame, Sectored Proton Fluxes, Hourly Averages
Hourly-averaged sectored proton fluxes from the MF Spectrum Analyzer of the ACE/EPAM LEFS60 instrument. All energies thresholds take into account the incident particle type, shielding, and inactive dead-layer of the solid state detector. All fluxes are background corrected and are in the solar wind rest frame.
ACE Solar Wind Electron, Proton, and Alpha Monitor (SWEPAM), Key Parameter, K1, Preliminary Browse Data
ACE Solar Wind Electron Proton Alpha Monitor (SWEPAM), Key Parameter, K1, Browse Data is designed for monitoring large scale particle and field behavior and for selecting interesting time periods. The data is automatically generated from the spacecraft data stream using simple algorithms provided by the instrument teams. It is not routinely checked for accuracy and is subject to revision. Use this data at your own risk, and consult with the appropriate instrument teams about citing it. SWEPAM browse data is not validated by the experimenters and should not be used except for preliminary examination prior to detailed Studies. See: https://izw1.caltech.edu/ACE/.
ACE Electron Proton Alpha Monitor (EPAM) LEFS150 MFSA, Solar Wind Frame, Sectored Proton Fluxes, Hourly Averages
Hourly-averaged sectored proton fluxes from the MF Spectrum Analyzer of the ACE/EPAM LEFS150 instrument. All energies thresholds take into account the incident particle type, shielding, and inactive dead-layer of the solid state detector. All fluxes are background corrected and are in the solar wind rest frame.
ACE Electron Proton Alpha Monitor (EPAM) LEFS60 MFSA, Solar Wind Frame, Sectored Z>1 Ion Fluxes, Daily Averages
Daily-averaged sectored Z>1 ion fluxes from the MF Spectrum Analyzer of the ACE/EPAM LEFS60 instrument. All energies thresholds take into account the incident particle type, shielding, and inactive dead-layer of the solid state detector. All fluxes are background corrected and are in the solar wind rest frame.
ISEE 1 Fast Plasma Experiment Solar Wind Weimer Propagated 60 s Resolution Data in GSM Coordinates
ISEE-1 Weimer propagated solar wind data and linearly interpolated to have the measurements on the minute at 60 s resolution FPE data in GSM coordinates. This data set consists of propagated solar wind data that has first been propagated to a position just outside of the nominal bow shock (about 17, 0, 0 Re) and then linearly interpolated to 1 min resolution using the interp1.m function in MATLAB. The input data for this data set is a 1 min resolution processed solar wind data constructed by Dr. J.M. Weygand. The method of propagation is similar to the minimum variance technique and is outlined in Dan Weimer et al. [2003; 2004]. The basic method is to find the minimum variance direction of the magnetic field in the plane orthogonal to the mean magnetic field direction. This minimum variance direction is then dotted with the difference between final position vector minus the original position vector and the quantity is divided by the minimum variance dotted with the solar wind velocity vector, which gives the propagation time. This method does not work well for shocks and minimum variance directions with tilts greater than 70 degrees of the sun-earth line. This data set was originally constructed by Dr. J.M. Weygand for Prof. R.L. McPherron, who was the principle investigator of two National Science Foundation studies: GEM Grant ATM 02-1798 and a Space Weather Grant ATM 02-08501. These data were primarily used in superposed epoch studies References: Weimer, D. R. (2004), Correction to ‘‘Predicting interplanetary magnetic field (IMF) propagation delay times using the minimum variance technique,’’ J. Geophys. Res., 109, A12104, doi:10.1029/2004JA010691. Weimer, D.R., D.M. Ober, N.C. Maynard, M.R. Collier, D.J. McComas, N.F. Ness, C. W. Smith, and J. Watermann (2003), Predicting interplanetary magnetic field (IMF) propagation delay times using the minimum variance technique, J. Geophys. Res., 108, 1026, doi:10.1029/2002JA009405.
ACE Electron Proton Alpha Monitor (EPAM) LEMS30 MFSA, Solar Wind Frame, Sectored Z>1 Ion Fluxes, Hourly Averages
Hourly-averaged sectored Z>1 ion fluxes from the MF Spectrum Analyzer of the ACE/EPAM LEMS30 instrument. All energies thresholds take into account the incident particle type, shielding, and inactive dead-layer of the solid state detector. All fluxes are background corrected and are in the solar wind rest frame.
ACE Electron Proton Alpha Monitor (EPAM) LEFS150 MFSA, Solar Wind Frame, Sectored Electron Fluxes, 17 min Averages
17-min-averaged sectored electron fluxes from the MF Spectrum Analyzer of the ACE/EPAM LEFS150 instrument. All energies thresholds take into account the incident particle type, shielding, and inactive dead-layer of the solid state detector. All fluxes are background corrected and are in the solar wind rest frame.
ACE Electron Proton Alpha Monitor (EPAM) LEFS/LEMS MFSA, Solar Wind Frame, Spin-Averaged Electron Fluxes, Hourly Averages
Hourly-averaged electron fluxes from the MF Spectrum Analyzer of the ACE/EPAM instrument. All energies thresholds take into account the incident particle type, shielding, and inactive dead-layer of the solid state detector. All fluxes are background corrected and are in the solar wind rest frame.
ACE Electron Proton Alpha Monitor (EPAM) LEMS120 MFSA, Solar Wind Frame, Sectored Proton Fluxes, Hourly Averages
Hourly-averaged sectored proton fluxes from the MF Spectrum Analyzer of the ACE/EPAM LEMS120 instrument. All energies thresholds take into account the incident particle type, shielding, and inactive dead-layer of the solid state detector. All fluxes are background corrected and are in the solar wind rest frame.
ACE Electron Proton Alpha Monitor (EPAM) LEMS30 MFSA, Solar Wind Frame, Sectored Proton Fluxes, Daily Averages
Daily-averaged sectored proton fluxes from the MF Spectrum Analyzer of the ACE/EPAM LEMS30 instrument. All energies thresholds take into account the incident particle type, shielding, and inactive dead-layer of the solid state detector. All fluxes are background corrected and are in the solar wind rest frame.
ACE Electron Proton Alpha Monitor (EPAM) LEFS/LEMS MFSA, Solar Wind Frame, Spin-Averaged Proton Fluxes, Daily Averages
Daily-averaged proton fluxes from the MF Spectrum Analyzer of the ACE/EPAM instrument. All energies thresholds take into account the incident particle type, shielding, and inactive dead-layer of the solid state detector. All fluxes are background corrected and are in the solar wind rest frame.
ACE Electron Proton Alpha Monitor (EPAM) LEFS150 MFSA, Solar Wind Frame, Sectored Proton Fluxes, 17 min Averages
17-min-averaged sectored proton fluxes from the MF Spectrum Analyzer of the ACE/EPAM LEFS150 instrument. All energies thresholds take into account the incident particle type, shielding, and inactive dead-layer of the solid state detector. All fluxes are background corrected and are in the solar wind rest frame.
APOLLO 15 ALSEP/SWS SOLAR WIND 28-SEC RESOLUTION TABLES V1.0
This data set contains daily tables of time ordered, 28-second-resolution plasma parameters, mainly of the solar wind, as observed on the Moon at the Apollo 15 ALSEP site by the Apollo 15 Solar Wind Spectrometer from 31 July 1971 through 30 June 1972.
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