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1) ISEE 1 FPE plasma parameters, 6 Re to bow shock maxmize
Resource ID:spase://VMO/NumericalData/ISEE1/FPE/PT1M
Start:1977-10-29 00:00:00 Observatory:ISEE 1 Cadence:1 minute
Stop:1979-01-19 00:00:00 Instrument:ISEE 1 Fast Plasma Experiment (FPE) and Solar Wind Ion Experiment (SWE) Resource:NumericalData
TBD

2) ISEE 1 Solar Wind Analyzer 24-s Plasma Parameters maxmize
Resource ID:spase://VMO/NumericalData/ISEE1/FPE/PT24S
Start:1977-10-30 00:00:00 Observatory:ISEE 1 Cadence:24 seconds
Stop:1984-01-30 00:00:00 Instrument:ISEE 1 Fast Plasma Experiment (FPE) and Solar Wind Ion Experiment (SWE) Resource:NumericalData
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).

3) ISEE 1 magnetometer 1-min data at CDAWeb maxmize
Resource ID:spase://VMO/NumericalData/ISEE1/MAG/PT1M
Start:1977-10-22 21:04:19 Observatory:ISEE 1 Cadence:1 minute
Stop:1987-09-25 16:10:30 Instrument:ISEE 1 Fluxgate Magnetometer, Tri-axial Resource:NumericalData
This data set contains magnetic field component and magnitude averages every minute, with components given in spacecraft, GSE and GSM coordinates. Standard deviations in the averages are given, as are differences between the averages and model field vectors. Geocentric (GSE and GSM) spacecraft position information is given, as is ISEE1-ISEE2 separation vector information. ISEE 1 spin vector direction and ISEE 1 velocity vector information, relative to the Earth and to ISEE 2, are given. Miscellaneous other parameters are also given. Data are accessible as plots, lists and files from CDAWeb, and as CDF files from CDAWeb's ftp area.

4) ISEE 1 magnetometer 4-sec data maxmize
Resource ID:spase://VMO/NumericalData/ISEE1/MAG/PT4S
Start:1977-10-22 21:04:19 Observatory:ISEE 1 Cadence:4 seconds
Stop:1987-09-25 16:10:30 Instrument:ISEE 1 Fluxgate Magnetometer, Tri-axial Resource:NumericalData
4-sec vector magnetic field values recorded by the NASA ISEE-1 satellite, in spacecraft coordinates (close to GSE), available from UCLA and CDAWeb value-added interfaces and, via ftp, in binary from UCLA and in CDF from CDAWeb. (This descriptor updated, 6/20110, by J.King, to reflect CDAWeb accessibility and to insert CDAWeb parameter keys.)

5) ISEE1 PWI Spectrum Analyzer - Rapid Sample maxmize
Resource ID:spase://VWO/NumericalData/ISEE1/PWE/SA-rapid.PT0.125S
Start:1977-10-27 00:00:00 Observatory:ISEE 1 Cadence:0.125 seconds
Stop:1987-09-26 06:07:59 Instrument:ISEE-1 Plasma wave experiment Resource:NumericalData
'The ISEE-1 and -2 Plasma Wave Investigation' D. A. Gurnett, F. L. Scarf, R. W. Fredricks, and E. J. Smith, IEEE Transactions on Geoscience Electronics, Vol. GE-16, p. 225-230, 1978. The International Sun-Earth Explorer (ISEE) Program consisted of three satellites intended to study the Earth's magnetosphere and the solar wind. ISEE-1 and ISEE-2 were launched on October 22, 1977 into highly elliptical geocentric orbits. The satellites passed through the magnetosphere and into the magnetosheath during each orbit. ISEE-3 was launched on August 12, 1978 and subsequently inserted into a 'halo orbit' about the the libration point situated about 240 earth radii (Re) upstream between the earth and the sun. Plasma passing this point arrives at the Earth about one hour later where it may cause changes that can be observed by ISEE 1 and ISEE-2. These two spacecraft, separated by a variable distance and with similar instrument complements, were intended to resolve the space-time ambiguity associated with measurements by a single spacecraft on thin boundaries which may be in motion such as the bow shock and the magnetopause. ISEE-1 and ISEE-3 were the principal U. S. contributions to the International Magnetospheric Study. ISEE-2 was built and managed by the European Space Agency. In September 1982 ISEE-3 was diverted from its 'halo orbit' to explore the earth's deep tail region through much of 1983 on its way to an encounter with the comet Giacobini Zinner in September 1985. ISEE-1 had a complement of thirteen experiments to measure the waves, fields, plasma, and particles. The University of Iowa Plasma Wave Instrument (PWI) was one of these thirteen. The ISEE-1 plasma waves instrument provided a comprehensive determination of wave characteristics over a broad frequency range, including high-frequency resolution spectrum scans, simultaneous high-time resolution electric and magnetic frequency spectrum measurements, wave normal and Poynting flux measurements, and wide-band waveform measurements. PWI sampled the environment using three electric dipole antennas with lengths of 215, 73.5, and 0.61 meters for electric-field measurements, and a triaxial search coil antenna with three 16-in high permeability mu-metal cores each wound with 10,000 turns of wire and a preamplifier for magnetic-field measurements. The experiment's main electronics consisted of four main elements: 1) a narrow-band sweep frequency receiver, 2) a pair of high time resolution spectrum analyzers, 3) a wave normal analyzer, and 4) an analog waveform receiver (also called a wide-band receiver). These elements could be electrically connected to the six antennas in various combinations in flight. Data for this file originate with an electric antenna and were measured via the Electric Spectrum Analyzer (ESA). The PWI ESA was designed to provide high time resolution spectrum measurements for resolving wave emissions that are bursty or of a nonlinear nature. The ESA was a 20-channel analyzer covering the range from 5.62 Hz to 311 kHz. It had a relatively coarse frequency resolution, with four frequency channels per decade and bandwidths of +/-15 percent up to 10 kHz and +/-7.5 percent for 10 kHz and above. The ESA was nominally intended for electric field measurements, though 2.2 percent of all ESA measurements were made using the Z-axis magnetic search coil. The ISEE spacecraft collected two separate data products with the PWI ESA. 1) A full frequency range 20-channel spectra and 2) a single-channel, rapid-sample series. The 'E_series' variable in this file provides ESA rapid-sample measurements. Full frequency range 20-channel spectra are provided in a companion file set. The rapid-sample series data were collected at 8-times the data rate of the 20-channel spectra, thus there are 32 samples per second in high rate telemetry mode and 4 per second in low-rate mode. Regardless of the telemetry mode, every 16 seconds the rapid sample channel is incremented until reaching the highest frequency band of the ESA (311 kHz), where it rolls over to the 5th band (56.2 Hz). Only the upper 16 channels of the ESA were sampled in this manner. Altogether this provides a 16-channel frequency sweep every 4 minutes and 16 seconds. Unlike the SFR data, the time to preform a complete frequency sweep is not affected by the telemetry mode, though the number of samples in a sweep does increase by a factor of 4. Given the slowly changing nature of the frequency channel compared to the sampling time these data are stored as a time series, with the current frequency relegated to a status variable. Nonetheless, frequency-time spectrograms may be constructed from these measurements if desired. For a detailed description of the Plasma Wave Instrument, the reader is referred to the IEEE Geoscience Electronics reference above. A common acronym for the plasma waves instrument in older documentation is GUM, which stands for for Gurnett Mother. Since this acronym is not easily recognizable by the space physics community and since no official acronym is provided in the instrument paper, the more common short hand 'PWI' is used to refer to the Plasma Wave Instrument in this archive.

6) ISEE 1 Plasma Wave Instrument Spectrum Analyzer Spectrogram Plots maxmize
Resource ID:spase://VWO/DisplayData/ISEE1/PWE/SA.PT12H
Start:1977-10-23 00:00:00 Observatory:ISEE 1 Cadence:
Stop:1987-09-26 23:59:59 Instrument:ISEE-1 Plasma wave experiment Resource:DisplayData
This dataset contains dynamic spectrogram PNG plots of the ISEE-1/PWI Spectrum Analyzer data. Each plot spans 12 hours. The dataset consists of files from 0-12UT and 12-24UT. These data were obtained from the Ev long wire antenna in the spin plane and the Bz search coil along the spin axis. Each image consists of two panels. The title above the upper panel is "ISEE-1 PWI Spectrum Analyzer Ev Antenna and Bz Search Coil". Each panel is a plot of the power spectral density of received signal (color scale) as a function of operating frequency (in a logarithmic scale on the vertical axis) and time (horizontal axis). The upper panel is a plot of Electric Spectral Density (SD) the lower plot is Magnetic SD. Beneath the time labels on the horizontal axis of the spectrograms are ephemeris data: position of the spacecraft in radial distance (Earth radii), geomagnetic latitude, magnetic local time, and McIlwain L-shell. Overlaid on the upper plot are traces of the electron cyclotron frequencies. At the bottom of the image is the date, day number and time range. Located in the same directory are the daily ISEE-1 PWI Sweep Frequency Receiver (SFR) spectrograms.

7) ISEE1 PWI Spectrum Analyzer maxmize
Resource ID:spase://VWO/NumericalData/ISEE1/PWE/SA.PT1S
Start:1977-10-22 19:13:20 Observatory:ISEE 1 Cadence:1 second
Stop:1987-09-26 06:07:59 Instrument:ISEE-1 Plasma wave experiment Resource:NumericalData
'The ISEE-1 and -2 Plasma Wave Investigation' D. A. Gurnett, F. L. Scarf, R. W. Fredricks, and E. J. Smith, IEEE Transactions on Geoscience Electronics, Vol. GE-16, p. 225-230, 1978. The International Sun-Earth Explorer (ISEE) Program consisted of three satellites intended to study the Earth's magnetosphere and the solar wind. ISEE-1 and ISEE-2 were launched on October 22, 1977 into highly elliptical geocentric orbits. The satellites passed through the magnetosphere and into the magnetosheath during each orbit. ISEE-3 was launched on August 12, 1978 and subsequently inserted into a 'halo orbit' about the the libration point situated about 240 earth radii (Re) upstream between the earth and the sun. Plasma passing this point arrives at the Earth about one hour later where it may cause changes that can be observed by ISEE 1 and ISEE-2. These two spacecraft, separated by a variable distance and with similar instrument complements, were intended to resolve the space-time ambiguity associated with measurements by a single spacecraft on thin boundaries which may be in motion such as the bow shock and the magnetopause. ISEE-1 and ISEE-3 were the principal U. S. contributions to the International Magnetospheric Study. ISEE-2 was built and managed by the European Space Agency. In September 1982 ISEE-3 was diverted from its 'halo orbit' to explore the earth's deep tail region through much of 1983 on its way to an encounter with the comet Giacobini Zinner in September 1985. ISEE-1 had a complement of thirteen experiments to measure the waves, fields, plasma, and particles. The University of Iowa Plasma Wave Instrument (PWI) was one of these thirteen. The ISEE-1 plasma waves instrument provided a comprehensive determination of wave characteristics over a broad frequency range, including high-frequency resolution spectrum scans, simultaneous high-time resolution electric and magnetic frequency spectrum measurements, wave normal and Poynting flux measurements, and wide-band waveform measurements. PWI sampled the environment using three electric dipole antennas with lengths of 215, 73.5, and 0.61 meters for electric-field measurements, and a triaxial search coil antenna with three 16-in high permeability mu-metal cores each wound with 10,000 turns of wire and a preamplifier for magnetic-field measurements. The experiment's main electronics consisted of four main elements: 1) a narrow-band sweep frequency receiver, 2) a pair of high time resolution spectrum analyzers, 3) a wave normal analyzer, and 4) an analog waveform receiver (also called a wide-band receiver). These elements could be electrically connected to the six antennas in various combinations in flight. Data for this file originate with the spectrum analyzers. The PWI Spectrum Analyzers were designed to provide high time resolution spectrum measurements for resolving wave emissions that are bursty or of a nonlinear nature. The pair consisted of a 20-channel analyzer covering the range from 5.62 Hz to 311 kHz, and a 14-channel analyzer covering the range from 5.62 Hz to 10 kHz. These analyzers have a relatively coarse frequency resolution, with four frequency channels per decade and bandwidths of +/-15 percent up to 10 kHz and +/-7.5 percent for 10 kHz and above. The center frequencies and bandwidths of the 20- and 14-channel analyzers are identical. The 20-channel analyzer was nominally intended for electric field measurements (which extend up to higher frequencies than the magnetic measurements), and the 14-channel analyzer was nominally intended for magnetic field measurements. All channels are sampled simultaneously so that electric-to-magnetic field ratios could be accurately determined. For a detailed description of the Plasma Wave Instrument, the reader is referred to the IEEE Geoscience Electronics reference above. A common acronym for the plasma waves instrument in older documentation is GUM, which stands for for Gurnett Mother. Since this acronym is not easily recognizable by the space physics community and since no official acronym is provided in the instrument paper, the more common short hand 'PWI' is used to refer to the Plasma Wave Instrument in this archive.

8) ISEE 1 Plasma Wave Instrument Sweep Frequency Receiver Spectrogram Plots maxmize
Resource ID:spase://VWO/DisplayData/ISEE1/PWE/SFR.P1D
Start:1977-10-26 00:00:00 Observatory:ISEE 1 Cadence:
Stop:1987-09-26 23:59:59 Instrument:ISEE-1 Plasma wave experiment Resource:DisplayData
This dataset contains dynamic spectrogram PNG plots of the ISEE1/PWI Sweep Frequency Receiver (SFR) data. Each plot spans one day. These data were obtained from the Ev long wire antenna in the spin plane and the Eu two-sphere antenna via the SFR receiver. The title above each spectrogram is "ISEE-1 PWI Sweep Frequency Receiver Ev and Eu Antennas". Each spectrogram is a plot of the power spectral density of received signal (color scale) as a function of operating frequency (in a logarithmic scale on the vertical axis) and time (horizontal axis). Beneath the time labels on the horizontal axis of the spectrograms are ephemeris data: position of the spacecraft in radial distance (Earth radii), geomagnetic latitude, magnetic local time, and McIlwain L-shell. Overlaid on each image are traces of the electron cyclotron frequencies. Located in the same directory are are the 12 hour ISEE-1 PWI Spectrum Analyzer (SA) spectrograms.

9) ISEE1 PWI Sweep Frequency Receiver maxmize
Resource ID:spase://VWO/NumericalData/ISEE1/PWE/SFR.PT32S
Start:1977-10-22 21:40:38 Observatory:ISEE 1 Cadence:32 seconds
Stop:1987-09-26 04:43:49 Instrument:ISEE-1 Plasma wave experiment Resource:NumericalData
'The ISEE-1 and -2 Plasma Wave Investigation' D. A. Gurnett, F. L. Scarf, R. W. Fredricks, and E. J. Smith, IEEE Transactions on Geoscience Electronics, Vol. GE-16, p. 225-230, 1978. The International Sun-Earth Explorer (ISEE) Program consisted of three satellites intended to study the Earth's magnetosphere and the solar wind. ISEE-1 and ISEE-2 were launched on October 22, 1977 into highly elliptical geocentric orbits. The satellites passed through the magnetosphere and into the magnetosheath during each orbit. ISEE-3 was launched on August 12, 1978 and subsequently inserted into a 'halo orbit' about the the libration point situated about 240 earth radii (Re) upstream between the earth and the sun. Plasma passing this point arrives at the Earth about one hour later where it may cause changes that can be observed by ISEE 1 and ISEE-2. These two spacecraft, separated by a variable distance and with similar instrument complements, were intended to resolve the space-time ambiguity associated with measurements by a single spacecraft on thin boundaries which may be in motion such as the bow shock and the magnetopause. ISEE-1 and ISEE-3 were the principal U. S. contributions to the International Magnetospheric Study. ISEE-2 was built and managed by the European Space Agency. In September 1982 ISEE-3 was diverted from its 'halo orbit' to explore the earth's deep tail region through much of 1983 on its way to an encounter with the comet Giacobini Zinner in September 1985. ISEE-1 had a complement of thirteen experiments to measure the waves, fields, plasma, and particles. The University of Iowa Plasma Wave Instrument (PWI) was one of these thirteen. The ISEE-1 plasma waves instrument provided a comprehensive determination of wave characteristics over a broad frequency range, including high-frequency resolution spectrum scans, simultaneous high-time resolution electric and magnetic frequency spectrum measurements, wave normal and Poynting flux measurements, and wide-band waveform measurements. PWI sampled the environment using three electric dipole antennas with lengths of 215, 73.5, and 0.61 meters for electric-field measurements, and a triaxial search coil antenna with three 16-in high permeability mu-metal cores each wound with 10,000 turns of wire and a preamplifier for magnetic-field measurements. The experiment's main electronics consisted of four main elements: 1) a narrow-band sweep frequency receiver, 2) a pair of high time resolution spectrum analyzers, 3) a wave normal analyzer, and 4) an analog waveform receiver (also called a wide-band receiver). These elements could be electrically connected to the six antennas in various combinations in flight. Data for this file originate with an electric antenna and were measured via the Sweep Frequency Receiver (SFR). The narrow-band sweep frequency receiver was intended to provide very high resolution spectrums with low time resolution for analyzing relatively steady narrow- band emissions such as upper hybrid resonance noise, electron plasma oscillations, and electron cyclotron harmonics. The receiver has 32 frequency steps in each of four bands covering the frequency range from approximately 100 Hz to 400 kHz. The frequency steps are logarithmically spaced with a frequency resolution of about 6.5 percent of the center frequency. The dynamic range of the receiver is 100 dB in the lowest three frequency bands, and 80 dB in the highest. Because the time resolution of the SFR is greater than the typical delay times for waves propagating between the two spacecraft, this receiver is only included on ISEE-1. For a detailed description of the Plasma Wave Instrument, the reader is referred to the IEEE Geoscience Electronics reference above. A common acronym for the plasma waves instrument in older documentation is GUM, which stands for for Gurnett Mother. Since this acronym is not easily recognizable by the space physics community and since no official acronym is provided in the instrument paper, the more common short hand 'PWI' is used to refer to the Plasma Wave Instrument in this archive.

10) ISEE 1 VES Electron Data at 9s or 18s maxmize
Resource ID:spase://VMO/NumericalData/ISEE1/VES/PT18S
Start:1977-10-29 00:00:00 Observatory:ISEE 1 Cadence:18 seconds
Stop:1979-06-03 00:00:00 Instrument:ISEE 1 Vector Electron Spectrometer (VES) Resource:NumericalData
This data set, held in CDAWeb as ISEE1_H0_FE, contains electron moments from the Vector Electron Spectrometer (VES), and spacecraft position vectors, at 9s or 18s resolution, depending on spacecraft telemetry rate. The data set also holds 1-min averages of the measured magnetic field vector. Electron moments include density, flow velocity, temperature and its anisotropy, and heat flux vector. Also given are the pressure tensor, its diagonalizing eigenvector, and the angle between its principal axis and the ambient magnetic field vector. These parameters are based on distributions accumulated in 3 sec but telemetered over 9s or 18s. Ancillary information given includes the spacecraft spin period, the spacecraft potential, the energy channels above this potential on which the moments for this record were based, and on/off flags for the Harvey and Mozer experiments.

11) ISEE-1 Linearly Interpolated 60 s Resolution Fast Plasma Experiment data in GSE Coordinates maxmize
Resource ID:spase://VMO/NumericalData/Weygand/ISEE1/FPE/Processed/GSE/PT60S
Start:1977-10-01 00:00:00 Observatory:ISEE 1 Cadence:60 seconds
Stop:1984-01-31 23:59:00 Instrument:ISEE 1 Fast Plasma Experiment (FPE) and Solar Wind Ion Experiment (SWE) Resource:NumericalData
ISEE-1 Fast Plasma Experiment data linearly interpolated to have the measurements on the minute at 60 s resolution data in GSE coordinates. This data set consists of processed solar wind data that has been linearly interpolated to 1 min resolution at the position of the spacecraft using the interp1.m function in MATLAB. 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 and cross correlation studies on solar wind.

12) ISEE-1 Linearly Interpolated 60 s Resolution Fast Plasma Experiment data in GSM Coordinates maxmize
Resource ID:spase://VMO/NumericalData/Weygand/ISEE1/FPE/Processed/GSM/PT60S
Start:1977-10-01 00:00:00 Observatory:ISEE 1 Cadence:60 seconds
Stop:1987-08-31 23:59:00 Instrument:ISEE 1 Fast Plasma Experiment (FPE) and Solar Wind Ion Experiment (SWE) Resource:NumericalData
ISEE-1 Fast Plasma Experiment data linearly interpolated to have the measurements on the minute at 60 s resolution data in GSM coordinates. This data set consists of processed solar wind data that has been linearly interpolated to 1 min resolution at the position of the spacecraft using the interp1.m function in MATLAB. 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 and cross correlation studies on solar wind.

13) ISEE-1 Fast Plasma Experiment Solar Wind Weimer Propagated 60 s Resolution Data in GSE Coordinates maxmize
Resource ID:spase://VMO/NumericalData/Weygand/ISEE1/FPE/Propagated.FPE/GSE/PT60S
Start:1977-10-01 00:00:00 Observatory:ISEE 1 Cadence:60 seconds
Stop:1984-01-31 23:59:00 Instrument:ISEE 1 Fast Plasma Experiment (FPE) and Solar Wind Ion Experiment (SWE) Resource:NumericalData
ISEE-1 Fast Plasma Experiment Weimer 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.

14) ISEE-1 Fast Plasma Experiment Solar Wind Weimer Propagated 60 s Resolution Data in GSM Coordinates maxmize
Resource ID:spase://VMO/NumericalData/Weygand/ISEE1/FPE/Propagated.FPE/GSM/PT60S
Start:1977-10-01 00:00:00 Observatory:ISEE 1 Cadence:60 seconds
Stop:1984-01-31 23:59:00 Instrument:ISEE 1 Fast Plasma Experiment (FPE) and Solar Wind Ion Experiment (SWE) Resource:NumericalData
ISEE-1 Weimer propagated solar wind data and linearly interpolated to have the measurements on the minute at 60 s resolution FPE data in GSM coordinates. This data set consists of propagated solar wind data that has first been propagated to a position just outside of the nominal bow shock (about 17, 0, 0 Re) and then linearly interpolated to 1 min resolution using the interp1.m function in MATLAB. The input data for this data set is a 1 min resolution processed solar wind data constructed by Dr. J.M. Weygand. The method of propagation is similar to the minimum variance technique and is outlined in Dan Weimer et al. [2003; 2004]. The basic method is to find the minimum variance direction of the magnetic field in the plane orthogonal to the mean magnetic field direction. This minimum variance direction is then dotted with the difference between final position vector minus the original position vector and the quantity is divided by the minimum variance dotted with the solar wind velocity vector, which gives the propagation time. This method does not work well for shocks and minimum variance directions with tilts greater than 70 degrees of the sun-earth line. This data set was originally constructed by Dr. J.M. Weygand for Prof. R.L. McPherron, who was the principle investigator of two National Science Foundation studies: GEM Grant ATM 02-1798 and a Space Weather Grant ATM 02-08501. These data were primarily used in superposed epoch studies References: Weimer, D. R. (2004), Correction to ??Predicting interplanetary magnetic field (IMF) propagation delay times using the minimum variance technique,?? J. Geophys. Res., 109, A12104, doi:10.1029/2004JA010691. Weimer, D.R., D.M. Ober, N.C. Maynard, M.R. Collier, D.J. McComas, N.F. Ness, C. W. Smith, and J. Watermann (2003), Predicting interplanetary magnetic field (IMF) propagation delay times using the minimum variance technique, J. Geophys. Res., 108, 1026, doi:10.1029/2002JA009405.

15) ISEE-1 Linearly Interpolated 60 s Resolution Tri-axial Fluxgate Magnetometer in GSE Coordinates maxmize
Resource ID:spase://VMO/NumericalData/Weygand/ISEE1/MAG/Processed/GSE/PT60S
Start:1977-10-01 00:00:00 Observatory:ISEE 1 Cadence:60 seconds
Stop:1984-01-31 23:59:00 Instrument:ISEE 1 Fluxgate Magnetometer, Tri-axial Resource:NumericalData
ISEE-1 linearly interpolated to have the measurements on the minute at 60 s resolution tri-axial fluxgate magnetometer data in GSE coordinates. This data set consists of processed solar wind data that has been linearly interpolated to 1 min resolution at the position of the spacecraft using the interp1.m function in MATLAB. 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 and cross correlation studies on solar wind.

16) ISEE-1 Linearly Interpolated 60 s Resolution Tri-axial Fluxgate Magnetometer in GSM Coordinates maxmize
Resource ID:spase://VMO/NumericalData/Weygand/ISEE1/MAG/Processed/GSM/PT60S
Start:1977-10-01 00:00:00 Observatory:ISEE 1 Cadence:60 seconds
Stop:1987-08-31 23:59:00 Instrument:ISEE 1 Fluxgate Magnetometer, Tri-axial Resource:NumericalData
ISEE-1 linearly interpolated to have the measurements on the minute at 60 s resolution tri-axial fluxgate magnetometer data in GSM coordinates. This data set consists of processed solar wind data that has been linearly interpolated to 1 min resolution at the position of the spacecraft using the interp1.m function in MATLAB. 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 and cross correlation studies on solar wind.

17) ISEE-1 Weimer Propagated 60 s Resolution Tri-axial Fluxgate Magnetometer in GSE Coordinates maxmize
Resource ID:spase://VMO/NumericalData/Weygand/ISEE1/MAG/Propagated.FPE/GSE/PT60S
Start:1977-10-01 00:00:00 Observatory:ISEE 1 Cadence:60 seconds
Stop:1984-01-31 23:59:00 Instrument:ISEE 1 Fast Plasma Experiment (FPE) and Solar Wind Ion Experiment (SWE) Resource:NumericalData
ISEE-1 Weimer propagated solar wind data and linearly interpolated to have the measurements on the minute at 60 s resolution tri-axial fluxgate magnetometer 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.

18) ISEE-1 Weimer Propagated 60 s Resolution Tri-axial Fluxgate Magnetometer in GSM Coordinates maxmize
Resource ID:spase://VMO/NumericalData/Weygand/ISEE1/MAG/Propagated.FPE/GSM/PT60S
Start:1977-10-01 00:00:00 Observatory:ISEE 1 Cadence:60 seconds
Stop:1984-01-31 23:59:00 Instrument:ISEE 1 Fast Plasma Experiment (FPE) and Solar Wind Ion Experiment (SWE) Resource:NumericalData
ISEE-1 Weimer propagated solar wind data and linearly interpolated to have the measurements on the minute at 60 s resolution tri-axial fluxgate magnetometer data in GSM coordinates. This data set consists of propagated solar wind data that has first been propagated to a position just outside of the nominal bow shock (about 17, 0, 0 Re) and then linearly interpolated to 1 min resolution using the interp1.m function in MATLAB. The input data for this data set is a 1 min resolution processed solar wind data constructed by Dr. J.M. Weygand. The method of propagation is similar to the minimum variance technique and is outlined in Dan Weimer et al. [2003; 2004]. The basic method is to find the minimum variance direction of the magnetic field in the plane orthogonal to the mean magnetic field direction. This minimum variance direction is then dotted with the difference between final position vector minus the original position vector and the quantity is divided by the minimum variance dotted with the solar wind velocity vector, which gives the propagation time. This method does not work well for shocks and minimum variance directions with tilts greater than 70 degrees of the sun-earth line. This data set was originally constructed by Dr. J.M. Weygand for Prof. R.L. McPherron, who was the principle investigator of two National Science Foundation studies: GEM Grant ATM 02-1798 and a Space Weather Grant ATM 02-08501. These data were primarily used in superposed epoch studies References: Weimer, D. R. (2004), Correction to ??Predicting interplanetary magnetic field (IMF) propagation delay times using the minimum variance technique,?? J. Geophys. Res., 109, A12104, doi:10.1029/2004JA010691. Weimer, D.R., D.M. Ober, N.C. Maynard, M.R. Collier, D.J. McComas, N.F. Ness, C. W. Smith, and J. Watermann (2003), Predicting interplanetary magnetic field (IMF) propagation delay times using the minimum variance technique, J. Geophys. Res., 108, 1026, doi:10.1029/2002JA009405.

19) ISEE-1 Solar Wind Weimer Propagation Details at 1 min Resolution maxmize
Resource ID:spase://VMO/NumericalData/Weygand/ISEE1/TAP/Propagated.FPE/GSE/PT60S
Start:1977-10-01 00:00:00 Observatory:ISEE 1 Cadence:60 seconds
Stop:1984-01-31 23:59:00 Instrument:ISEE 1 Fast Plasma Experiment (FPE) and Solar Wind Ion Experiment (SWE) Resource:NumericalData
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.

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