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342 results for “Solar Wind”
ICE SOLAR WIND PLASMA ELECTRON ANALYSER DATA V1.0
These data were obtained from the LANL plasma experiment on ICE (Principal Investigator: S.J. Bame assistance from K. Sofaly and S. Kedge). The instrument measures the 2-D electron distribution function in one spacecraft rotation (3 s) once every 24 s, by obtaining 16 evenly spaced energy spectra, each with 15 contiguous levels covering the energy range 8.5 eV to 1140 eV. From these 2-D distributions the density, velocity, and temperature of the electrons are then derived. A 2-D temperature matrix is calculated which is subsequently diagonalized. Then nominally the maximum temperature corresponds to the parallel temperature and the minimum temperature corresponds to the perpendicular temperature. This is done independently of the magnetic field measurements however, the direction of maximum temperature determined in this manner is usually found to be within 15 degrees of the magnetic field direction inferred from the magnetometer measurements. The time resolution is 24 sec from the start of Day 253 (September 10) until Day 255 (September 12), 18:38. At that time the bit rate dropped from 1024 to 512 bps, and the nominal time resolution went to 48 sec.
ACE Electron Proton Alpha Monitor (EPAM) LEFS150 MFSA, Solar Wind Frame, Sectored Proton Fluxes, Daily Averages
Daily-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) LEMS30 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 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.
Apollo 12 Solar Wind Measurements at the Lunar Surface 1-HR Data
This data set contains hourly averaged plasma parameters from the Apollo 12 Solar Wind Spectrometer. Four sets of hourly averaged parameters are computed, using as input data -- (1) all fine-time scale parameters (FTSP), (2) all FTSP computed from spectra with small rms error on curve fitting and thermal speeds less than one-half the bulk velocity, (3) all FTSP computed from spectra that satisfy the requirements of criterion 2 as well as having only one flow angle that can be directly measured, and (4) all FTSP computed from spectra that satisfy the requirements of criterion 2 as well as having both flow angles directly measureable. Contained in each of the 4 sets of averages are the proton density, alpha-to-proton ratio, bulk speed, angle of flow, number of spectra, and rms deviations of each average.
ACE Electron Proton Alpha Monitor (EPAM) LEFS60 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 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.
ROSETTA-ORBITER SOLAR WIND RPCIES 2 RVM1 V1.0
This dataset contains EDITED RAW DATA of the Rosetta RPCIES instrument taken during the Rendezvous Manoeuvre 1 (RVM1). Included are the data taken between 29 Nov 2010 and 30 Nov 2010.
ACE Electron Proton Alpha Monitor (EPAM) LEMS120 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 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.
IMP-8 PLS Solar Wind Weimer Propagated 60 s Resolution Data in GSE Coordinates
IMP-8 PLS propagated solar wind data and linearly interpolated to have the measurements on the minute at 60 s resolution data in GSE 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) LEFS60 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 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.
APOLLO 15 ALSEP/SWS SOLAR WIND 1-HR AVG TABLES V1.0
This data set contains tables of time ordered, hourly averaged 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.
ACE Electron Proton Alpha Monitor (EPAM) LEFS/LEMS MFSA, Solar Wind Frame, Spin-Averaged Z>1 Ion Fluxes, Daily Averages
Daily-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) LEFS150 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 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, 17 min Averages
17-min-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.
Wind Solar Wind Experiment (SWE) Electron Moments Parameters (6-12s rate) (1994-2001)
Wind SWE 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. 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 temperaturetensor. 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 inconjunction 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 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.
ROSETTA-ORBITER SOLAR WIND RPCIES 2 CR2 V1.0
This dataset contains EDITED RAW DATA of cruise 2 phase. Included are the data taken from 03 October 2005 to 7 March 2006.
Geotail Solar Wind Weimer Propagation Details at 1 min Resolution
Geotail Weimer propagated solar wind data using CPI 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 SWICS 2.0 Solar Wind Protons 12-min Data
The SWICS 12-minute proton data contains densities, speeds, and thermal speeds from the beginning of the mission up to the present day. The densities have been cross-calibrated to the proton monitors ACE/SWEPAM and WIND/SWE, and represent a continuous data set that can be used in conjunction with other SWICS data, or as a stand-alone measurement. For details on the SWICS proton data, see the release notes provided by the instrument team: http://www.srl.caltech.edu/ACE/ASC/DATA/level2/ssprotons/swics_protons_release_notes.txt
ACE Electron Proton Alpha Monitor (EPAM) LEFS60 MFSA, Solar Wind Frame, Sectored Proton Fluxes, Daily Averages
Daily-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.
Wind Solar Wind Experiment (SWE) 92-sec Definitive Solar Wind Proton Data
SWE is a comprehensive plasma instrument for the WIND spacecraft, see K.W.Ogilvie, et al., Space Sci. Rev., 71, 55-77, 1995. This product provides solar wind proton parameters, including anisotropic temperatures, derived by non-linear fitting of the measurements and with moment techniques. Data reported within this product 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 were 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.
Geotail Solar Wind Weimer Propagation Details at 1 min Resolution
Geotail Weimer propagated solar wind data using LEP 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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