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CDAWeb Served Heliophysics Datasets Beginning with 'W'

WILD2_HELIO1DAY_POSITION: Position in heliocentric coordinates from SPDF Helioweb - Natalia Papitashvili (NASA/GSFC/SPDF)
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. Szabo (NASA/GSFC)
WI_H0_SWE: Wind SWE (Solar Wind Experiment), 6 - 12 sec Solar Wind Electron Moments - K. Ogilvie (GSFC Code 692)
WI_H0_WAV: Wind Radio/Plasma Wave, (WAVES) High Res. Plasma Density - M. L. Kaiser (GSFC)
WI_H1_SWE: Wind Solar Wind Experiment, 92-sec Solar Wind Alpha and Proton Anisotropy Analysis - K. Ogilvie (NASA GSFC)
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. Szabo (NASA/GSFC)
WI_H3_SWE: Wind Solar Wind Experiment (SWE), 9 sec solar wind electron pitch-angle distributions at 12 sec cadence - K. Ogilvie (NASA/GSFC)
WI_H4_SWE: Wind Solar Wind Experiment (SWE), 3 sec solar wind electron pitch-angle distributions at 6-12 sec cadence - K. Ogilvie (NASA/GSFC)
WI_H5_SWE: Wind Solar Wind Experiment (SWE), 9 sec solar wind electron moments at 12 sec cadence - K. Ogilvie (NASA/GSFC)
WI_K0_3DP: Wind 3-D Plasma Analyzer, Key Parameters - R. Lin/S. Bale (UC Berkeley)
WI_K0_EPA: Wind Energetic Particle Acceleration Composition Transport, Key Parameters - 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 Maryland)
WI_K0_SPHA: Wind Spin Phase
WI_K0_SWE: Wind SWE (Solar Wind Experiment), Key Parameters - K. Ogilvie (NASA GSFC)
WI_K0_WAV: Wind Radio/Plasma Wave, (WAVES) Key Parameters - M. L. Kaiser (GSFC)
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_L2-5MIN-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-HE2PLUS-3MIN_SMS-STICS-MAGNETOSPHERE: Solar Wind and Suprathermal Ion Composition Instrument, Key Parameters - G. Gloeckler (U of Maryland)
WI_L2-HE2PLUS-3MIN_SMS-STICS-SOLARWIND: Solar Wind and Suprathermal Ion Composition Instrument, Key Parameters - G. Gloeckler (U of Maryland)
WI_L2-HPLUS-3MIN_SMS-STICS-MAGNETOSPHERE: Solar Wind and Suprathermal Ion Composition Instrument, Key Parameters - G. Gloeckler (U of Maryland)
WI_L2-HPLUS-3MIN_SMS-STICS-SOLARWIND: Solar Wind and Suprathermal Ion Composition Instrument, Key Parameters - G. Gloeckler (U of Maryland)
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 (SWE), 9 sec solar wind electron pitch-angle distribution averages - K. Ogilvie (NASA/GSFC)
WI_M2_SWE: Wind Solar Wind Experiment (SWE), 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)

WILD2_HELIO1DAY_POSITION
Description
No TEXT global attribute value.
 
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WI_AT_DEF (spase://VSPO/NumericalData/Wind/Attitude/Definitive/PT10M)
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
 
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WI_AT_PRE (spase://VSPO/NumericalData/Wind/Attitude/Predicted/PT10M)
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
 
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WI_EHPD_3DP (spase://VSPO/NumericalData/Wind/3DP/EESA_HIGH/PD/PT24S)
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.
 
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WI_EHSP_3DP (spase://VSPO/NumericalData/Wind/3DP/EESA_HIGH/SP/PT24S)
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.
 
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WI_ELM2_3DP (spase://VSPO/NumericalData/Wind/3DP/EESA_LOW/Moments)
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.
 
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WI_ELPD_3DP (spase://VSPO/NumericalData/Wind/3DP/ELPD/PT96S)
Description
Wind 3dp, EESA Low electron pitch angle distributions with ion-derived moments
 
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WI_ELSP_3DP (spase://VSPO/NumericalData/Wind/3DP/EESA_LOW/SP/PT24S)
Description
Wind 3dp, EESA Low omni directional electron energy spectra
 
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WI_EMFITS_E0_3DP (spase://VSPO/NumericalData/Wind/3DP/EMFITS/PT100S)
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.
 
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WI_EM_3DP (spase://VSPO/NumericalData/Wind/3DP/EM/PT3S)
Description
Wind 3dp, EESA LOW 1 spin resolution Plasma ( electron ) moments (computed on
spacecraft)
Modification History
Version 3 Product, August 2005
 
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WI_EPACT_STEP-DIFFERENTIAL-ION-FLUX-1HR (spase://VSPO/NumericalData/Wind/EPACT/STEP/DifferentialFlux/Ion/PT1H)
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 
 
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WI_EPACT_STEP-DIRECTIONAL-DIFF-CNO-FLUX-10MIN (spase://VSPO/NumericalData/Wind/EPACT/STEP/Directional/DifferentialFlux/CNO/PT10M)
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. 
 
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WI_EPACT_STEP-DIRECTIONAL-DIFF-FE-FLUX-10MIN (spase://VSPO/NumericalData/Wind/EPACT/STEP/Directional/DifferentialFlux/Iron/PT10M)
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. 
 
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WI_EPACT_STEP-DIRECTIONAL-DIFF-H-FLUX-10MIN (spase://VSPO/NumericalData/Wind/EPACT/STEP/Directional/DifferentialFlux/Hydrogen/PT10M)
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. 
 
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WI_EPACT_STEP-DIRECTIONAL-DIFF-HE-FLUX-10MIN (spase://VSPO/NumericalData/Wind/EPACT/STEP/Directional/DifferentialFlux/Helium/PT10M)
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. 
 
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WI_H0_MFI (spase://VSPO/NumericalData/Wind/MFI/PT03S)
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                    
 
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WI_H0_SWE (spase://VSPO/NumericalData/Wind/SWE/H0/PT06S)
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
 
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WI_H0_WAV (spase://VSPO/NumericalData/Wind/WAVES/PT18S)
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
 
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WI_H1_SWE (spase://VSPO/NumericalData/Wind/SWE/Definitive/PT92S)
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.
 
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WI_H1_WAV (spase://VSPO/NumericalData/Wind/WAVES/DS/PT1M)
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
 
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WI_H2_MFI (spase://VSPO/NumericalData/Wind/MFI/PT0.092S)
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                    
 
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WI_H3_SWE (spase://VSPO/NumericalData/Wind/SWE/H3/PT12S)
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
 
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WI_H4_SWE (spase://VSPO/NumericalData/Wind/SWE/H4/PT06S)
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
 
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WI_H5_SWE (spase://VSPO/NumericalData/Wind/SWE/H5/PT12S)
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 12/10/2009.
 
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WI_K0_3DP (spase://VSPO/NumericalData/Wind/3DP/KP/PT92S)
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 
 
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WI_K0_EPA (spase://VSPO/NumericalData/Wind/EPACT/PT92S)
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
Modified May 18, 1995
Added better TEXT description June 30, 2010
 
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WI_K0_GIFWALK
Description
Pre-generated PWG plots
 
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WI_K0_MFI (spase://VSPO/NumericalData/Wind/MFI/KeyParameters/PT92S)
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 
 
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WI_K0_SMS (spase://VSPO/NumericalData/Wind/SMS/KP/PT4H)
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
 
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WI_K0_SPHA (spase://VSPO/NumericalData/Wind/Ephemeris/Spin/PT600S)
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
 
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WI_K0_SWE (spase://VSPO/NumericalData/Wind/SWE/KeyParameters/PT92S)
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.
 
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WI_K0_WAV (spase://VSPO/NumericalData/Wind/WAVES/KeyParameters/PT18S)
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
 
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WI_L2-1HOUR-SEP_EPACT-APE_B (spase://VSPO/NumericalData/Wind/EPACT/SEP/PT1H)
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 
 
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WI_L2-1HOUR-SEP_EPACT-LEMT (spase://VSPO/NumericalData/Wind/EPACT/LEMT/L2/PT1H)
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 
 
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WI_L2-5MIN-SEP_EPACT-LEMT (spase://VSPO/NumericalData/Wind/EPACT/LEMT/L2/PT5M)
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 
 
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WI_L2-HE2PLUS-3MIN_SMS-STICS-MAGNETOSPHERE
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
Version 01 Feb. 1996 - whm
 
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WI_L2-HE2PLUS-3MIN_SMS-STICS-SOLARWIND
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
Version 01 Feb. 1996 - whm
 
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WI_L2-HPLUS-3MIN_SMS-STICS-MAGNETOSPHERE
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
Version 01 Feb. 1996 - whm
 
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WI_L2-HPLUS-3MIN_SMS-STICS-SOLARWIND
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
Version 01 Feb. 1996 - whm
 
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WI_L3-DUSTIMPACT_WAVES (spase://VSPO/NumericalData/Wind/WAVES/DustImpact/PT1S)
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).
 
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WI_M0_SWE (spase://VSPO/NumericalData/Wind/SWE/M0/PT12S)
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
 
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WI_M2_SWE (spase://VSPO/NumericalData/Wind/SWE/M2/PT06S)
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
 
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WI_OR_DEF (spase://VSPO/NumericalData/Wind/Ephemeris/definitive/PT10M)
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 
 
Dataset in CDAWeb
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WI_OR_GIFWALK
Description
Pre-generated PWG plots
 
Dataset in CDAWeb
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WI_OR_PRE (spase://VSPO/NumericalData/Wind/Ephemeris/predicted/PT10M)
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 
 
Dataset in CDAWeb
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WI_PLSP_3DP (spase://VSPO/NumericalData/Wind/3DP/PLSP/PT24S)
Description
Wind 3dp, PESA Low (~24 sec resolution) energy spectra with ion moments 
 
Dataset in CDAWeb
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WI_PM_3DP (spase://VSPO/NumericalData/Wind/3DP/PM/PT03S)
Description
Wind 3dp, PESA LOW 1 spin resolution ion (proton and alpha) moments (computed on
spacecraft)
Modification History
Version 3 Product, August 2005
 
Dataset in CDAWeb
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WI_SFPD_3DP (spase://VSPO/NumericalData/Wind/3DP/SST_Foil/PD/PT24S)
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.
 
Dataset in CDAWeb
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WI_SFSP_3DP (spase://VSPO/NumericalData/Wind/3DP/SST_Foil/SP/PT24S)
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.
 
Dataset in CDAWeb
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WI_SOPD_3DP (spase://VSPO/NumericalData/Wind/3DP/SST_Open/PD/PT24S)
Description
Wind 3dp, SOPD
 
Dataset in CDAWeb
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WI_SOSP_3DP (spase://VSPO/NumericalData/Wind/3DP/SST_Open/SP/PT24S)
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.
 
Dataset in CDAWeb
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WI_STRAHL0_SWE (spase://VSPO/NumericalData/Wind/SWE/Strahl/PT12S)
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
 
Dataset in CDAWeb
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WI_SW-ION-DIST_SWE-FARADAY (spase://VSPO/NumericalData/Wind/SWE/Faraday-Cup/Ion-Dist/PT92S)
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.

 
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