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342 results for “Solar Wind”
VOYAGER 1 SOLAR WIND PLS FINE RES V1.0
Voyager 1 plasma data of the solar wind, fine resolution data.
VG1 JUP PLS DERIVED ION INBOUND SOLAR WIND 96SEC V1.0
Voyager 1 Plasma Experiment (PLS)averaged ion inbndswind 96 second data at Jupiter.
VOYAGER 2 SOLAR WIND PLS 1 HOUR AVERAGES V1.0
Voyager 2 plasma data of the solar wind, 1 hour averages.
VOYAGER 2 SOLAR WIND PLS 1 DAY AVERAGES V1.0
Voyager 2 plasma data of the solar wind, 1 day averages.
VG2 SAT PLS DERIVED ION SOLAR WIND 96SEC V1.0
not applicable
P11 SATURN SOLAR WIND CPI CRUISE 15 MIN COUNT DATA V1.0
Pioneer 11 cruise Charged Particle Instrument (CPI) 15 minute count data.
VOYAGER 2 SOLAR WIND PLS FINE RES V1.0
Voyager 2 plasma data of the solar wind, fine resolution data.
ULY JUPITER SOLAR WIND ION COMPOSITION SPECTROMETER NO DATA
No SWICS data were archived with PDS for the Ulysses Jupiter Encounter.
The correspondence of Pc5 waves at high latitude and in the solar wind during the solar cycle 23: Data of figures
<p>This deposit contains the data used in the publication in Journal of Geophysical Research: Space Physics, currently titled "The correspondence of Pc5 waves at high latitude and in the solar wind during the solar cycle 23". The paper associated with the data has been submitted on 19.12.2018, and this upload has been done to correspond with the data policy of the journal. The data will be made available through Zenodo after the paper has been accepted for publication or as required by the journal.</p> <p>The steps required to produce this derived data set have been described in detail in the publication above.</p>
Wind Solar Wind Experiment (SWE) Averaged Electron Pitch Angle Distribution (6-12s rate)
Averaged Wind SWE electron pitch angle data (6-12 seconds rate) from an earlier mode (VEIS-era) of the electron instrument. 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, 1995). 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).
Wind Solar Wind Weimer Propagation Details at 1 min Resolution
Wind Weimer propagated solar wind data and linearly interpolated time delay, cosine angle, and goodness information of propagated data at 1 min Resolution. 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) LEFS150 MFSA, Solar Wind Frame, Sectored Electron Fluxes, Daily Averages
Daily-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.
Wind Solar Wind Experiment (SWE) Electron Pitch-Angle Distributions (6-12s rate) (VEIS-era Mode)
Wind SWE electron pitch angle product providing electron fluxes at 30 directional bins relative to the instantaneous magnetic field direction at 16 different energy levels from the old mode (VEIS-era) of the electron instrument. 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.
STEREO-A In-Situ Measurements of Particles and CME Transients (IMPACT) Solar Wind Electron Analyzer (SWEA) Spectra
STEREO Ahead In-situ Measurements of Particles and CME Transients, IMPACT, Solar Wind Electron Analyzer, SWEA, Level 1 Data
STEREO-B In-Situ Measurements of Particles and CME Transients (IMPACT) Solar Wind Electron Analyzer (SWEA) Spectra
STEREO Behind In-situ Measurements of Particles and CME Transients, IMPACT, Solar Wind Electron Analyzer, SWEA, Level 1 Data
ISEE 1 Solar Wind Analyzer 24-s Plasma Parameters
This data set contains 24s (fast data rate) or 48s (slow rate) solar wind ion plasma parameters obtained during 1977-1983 solar wind seasons (~July - ~January) when the spacecraft's local time of apogee was on the Earth's dayside. Plasma parameters include ion density, flow speed, flow longitude and latitude angles, perpendicular (minimum) and parallel (maximum) temperatures, and alpha-to-proton density ratio. Data are available through the CDAWeb interface and, as daily files via ftp, in ASCII from nssdcftp and in CDF from CDAWeb's ftp area. The data are from LANL's Cross-Fan Solar Wind Ion Experiment, a companion to LANL's Fast Plasma Analyzer (FPE).
ISEE 1 Solar Wind Weimer Propagation Details at 1 min Resolution
ISEE-1 Weimer propagated solar wind data and linearly interpolated time delay, cosine angle, and goodness information of propagated data at 1 min Resolution. 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) LEFS/LEMS MFSA, Solar Wind Frame, Spin-Averaged Z>1 Ion Fluxes, Hourly Averages
Hourly-averaged ion 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) LEFS/LEMS MFSA, Solar Wind Frame, Spin-Averaged Proton Fluxes, 17 min Averages
17-min-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.
ISEE-3 Solar Wind Weimer Propagation Details at 1 min Resolution
ISEE-3 Weimer propagated solar wind data and linearly interpolated time delay, cosine angle, and goodness information of propagated data at 1 min Resolution. 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.
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