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1) | IMP 8 bow shock crossings | |||||||||||||||||
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Resource ID:spase://VMO/Catalog/BS_IMP8 | ||||||||||||||||||

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A complete list of bow shock crossings observed by IMP 8 spacecraft. The shock crossings were manually identified in magnetic field and/or thermal plasma measurements by J. Merka, A. Szabo, K. Paularena, J. Richardson, and T. Narock. Each identified crossing was reviewed by at least two persons from the team. Upstream parameters are as measured by IMP 8 on the solar wind side of the shock, typically over a few-minute interval judged by the IMP field and plasma teams as stable. For multiple-shock records, all upstream parameters are for the first shock crossing. Downstream parameters are as measured by IMP 8 on the magnetosheath side of the shock, typically over a few-minute interval. For a multiple-shock records, all downstream parameters are for the first shock crossing if possible. |

2) | IMP 8 CPME EPE MAG PLS Merge Data Set | |||||||||||||||||
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Resource ID:spase://VEPO/NumericalData/IMP8/CPME/EPE/PT20S | ||||||||||||||||||

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This data set contains 20.48s IMP8 CPME and EPE energetic particle data, along with IMP8 magnetic field and plasma data to facilitate use of the particle data. CPME data consist of: spin-integrated, 20.48s resolution count rates of protons in ten energy channels (0.29-0.50 to 90-440 MeV), of alpha particles in six channels (0.59-1.14 to 28-52 MeV/n), of Z>=3 particles in five channels (0.70-1.45 to 6-105 MeV/n), of electrons in 3 channels (0.22-2.5 to 0.80-2.5 MeV), of protons and alpha particles mixed in two channels (>35, >50 MeV/n) and uncertainties in all the preceding 20-s rates; spin-integrated, 10.24s count rates of protons in three energy channels (0.29-0.50 to 0.96-2.00 MeV) and of electrons in the three energy channels given above, plus uncertainties and data quality flags for all these 10.24s rates; 10.24s count rates in 8 spin sectors for 0.29-0.50 MeV protons and for 0.22-2.50 MeV electrons and their uncertainties and dataquality flags; 20.48s count rates in 8 spin sectors for 0.59-1.14 and 1.8-4.2 MeV/n alpha particles and for 0.7-3.3 and 3.1-8.8 MeV/n Z>= 3 particles, and their uncertainties anddata quality flags. EPE data consist of 16-sectored, 20.48s counts (not rates) for Z>=1 particles in 0.05-0.22 and 0.22-0.80 MeV/n channels, for electrons in 0.03-0.10 and 0.10-0.20 MeV channels and for Z>=1, E>0.015 MeV/n particles and electrons mixed. Magnetic field data include GSE and GSM cartesian components and direction angles. Plasma data, mainly from the MIT Faraday Cup, include flow velocity, density and temperature. Better sources exist for those desiring only IMP8 magnetic field and/or plasma data. Data are available as daily gzipped ASCII files; spin- integrated, 20.48s CPME count rates are also available with display and subset capability via FTPBrowser. |

3) | IMP 8 CRNC hourly energetic electron fluxes | |||||||||||||||||
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Resource ID:spase://VEPO/NumericalData/IMP8/CRNC/Electrons_PT1H | ||||||||||||||||||

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This data set contains hourly, spin-averaged fluxes of electrons from the IMP8 Cosmic Ray Nuclear Composition experiment of U. Chicago and UNH. There are fluxes of electrons in three energy bins: 0.7-2.0, 2-12, 12-50 MeV. These fluxes were generated at GSFC/SPDF from count rates accessible from UNH. |

4) | IMP 8 CRNC hourly count rates of heavy nuclei | |||||||||||||||||
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Resource ID:spase://VEPO/NumericalData/IMP8/CRNC/Heavies_PT1H | ||||||||||||||||||

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This data set contains hourly, spin-averaged count rates of heavy nuclei, and of particles penetrating the anticoincidence sensor, from the IMP8 Cosmic Ray Nuclear Composition experiment of U. Chicago and UNH. Included are rates of CNO nuclei at E.LT.80 MeV/n and E.GT.80 MeV/n, of Z.GT.8 nuclei at "low" and "high" energies, and of penetrating particles (protons with E.GT.106 MeV, etc.) |

5) | IMP 8 CRNC hourly energetic alpha particle fluxes | |||||||||||||||||
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Resource ID:spase://VEPO/NumericalData/IMP8/CRNC/Helium_PT1H | ||||||||||||||||||

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This data set contains hourly, spin-averaged fluxes of alpha particles from the IMP8 Cosmic Ray Nuclear Composition experiment of U. Chicago and UNH. There are fluxes of alpha particles in 9 energy bins from 10.90-12.89 to 84.32-94.81 MeV/n. These fluxes were generated at GSFC/SPDF from count rates accessible from UNH. |

6) | IMP 8 CRNC 15-min PHA and coincidence mode counts | |||||||||||||||||
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Resource ID:spase://VEPO/NumericalData/IMP8/CRNC/PT15M | ||||||||||||||||||

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This 15-min-resolution data set consists of 5 count rates from the Low Energy Telescope, 8 count rates for the main telescope (MT), 4 counts of pulse height analyzed events in each of 4 MT coincidence modes, and 27 box counts corresponding to specific species and energy ranges associated with 3 of the MT coincidence modes. Actually the 13 referenced "count rates" are given as paired counts and accumulation times. Associated documentation suggests algorithms for computation of count rates and fluxes from the MT data given, for electrons in 3 energy bands (0.7-2.0, 2.0-12, 12-50 MeV), protons in 9 bands (11.24-20.00 MeV to 74.50-94.78 MeV), helium nuclei in 10 bands (10.90-12.89 MeV per n to 84.32-94.81 MeV per n), and CNO nuclei in 1 band (25 - 250 Mev per n). There are no azimuthally sectored data in this data set. The data are accessible via ftp and, with higher functionality, via FTPBrowser. |

7) | IMP 8 CRNC hourly energetic proton fluxes | |||||||||||||||||
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Resource ID:spase://VEPO/NumericalData/IMP8/CRNC/Protons_PT1H | ||||||||||||||||||

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This data set contains hourly, spin-averaged fluxes of protons from the IMP8. Cosmic Ray Nuclear Composition experiment of U. Chicago and UNH. There are are fluxes of protons in 9 energy bins from 11.24-12.62 to 74.50-94.78 MeV. These fluxes were generated at GSFC/SPDF from count rates accessible from UNH. |

8) | IMP 8 UMD EECA 10.92m Rates, PHA | |||||||||||||||||
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Resource ID:spase://VEPO/NumericalData/IMP8/EECA/PT11M | ||||||||||||||||||

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This data set, from the Electrostatic Energy-Charge Analyzer (EECA) part of the U. Maryland experiment on IMP 8, contains count rate and pulse height data enabling the computation of 10.92-min resolution fluxes of: singly ionized ions in 5 energy/charge windows of lower limits between 130 and 740 keV/Q; doubly charged ions in the same 5 keV/Q windows plus another at 65 keV/Q; ions with charge states between 5 and 8 in the same 6 keV/Q windows as for doubly charged ions plus another at 37 keV/Q; ions with charge states above about 10 at 37 and 65 keV/Q windows; 600-860 keV electrons. Some of the modes are spin integrated while others are given in 90 deg quadrants about the spacecraft spin vector (which is normal to the ecliptic plane). The data set was created at NSSDC from the U.Md.-provided "summary tapes" (NSSDC IDs SPHE-00170 and 73-078A-03C) by dropping engineering data, dropping data from the ULET portion of the overall experiment (the ULET instrument failed in 1978), and converting the remaining time, spacecraft position, and EECA instrument data from binary to ASCII representation. The data are available via ftp in 1- month files of variable lengths in the 3-6 MB size range. |

9) | IMP 8 Spacecraft Positions | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/IMP8/Ephemeris/PT12M | ||||||||||||||||||

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IMP-8 spacecraft positions in various coordinate systems |

10) | IMP 8 GME 30-min energetic particle rates and fluxes | |||||||||||||||||
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Resource ID:spase://VEPO/NumericalData/IMP8/GME/PT30M | ||||||||||||||||||

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This CDAWeb-accessible data set contains 30-minute, spin-averaged count rates and fluxes, and their statistical uncertainties, of energetic particles from the IMP8 GME experiment. Included are fluxes of: protons in 30 energy bins from 0.88-1.15 to 327-485 MeV; alpha particles in 21 energy bins from 1.14-1.36 to 63.3-81.0 MeV/n; and 0.3-18 MeV electrons. Also included are count rates for each of 7 sensors and for 11 multi-sensor coincidence modes. Proton and alpha particle fluxes, for every other energy bin, are given at the FTPBrowser and MSSP interfaces identified below. |

11) | IMP 8 MAG 320 msec GSE magnetic field data | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/IMP8/MAG/PT0.32S | ||||||||||||||||||

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Data consist of 320 ms magnetic field magnitude and Cartesian components. |

12) | IMP 8 MAG 15.36s Magnetic Field Measurements | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/IMP8/MAG/PT15.36S | ||||||||||||||||||

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IMP 8 magnetic field measurements from tri-axis magnetometer. Time resolution is 15.36 second. Data are based on a 2010 data reprocessing by the PI team. Parameter details below are based on the version of the data in CDAWeb. |

13) | IMP 8 MIT Full Resolution Definitive Interplanetary Plasma Data | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/IMP8/PLS/PT01M | ||||||||||||||||||

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The MIT Faraday cup experiment on IMP 8 measures currents from solar wind ions, and from these measurements we calculate the velocity, density, and temperature of the solar wind. The IMP 8 data files consist of fine resolution data (approximately 1 minute resolution). IMP 8 spins with a period of approximately 2.7s. The Faraday Cup (FC) instrument scans the solar wind distribution stepping through a contiguous set of energy windows, one step per spacecraft spin. The FC instrument divides the spin into thirty-two, 11.25 degree angular sectors and integrates the measured currents over different angular sectors depending upon the Mode in which the instrument is operating. The border between two of the 11.25 degree angular sectors lies on the Sun-spacecraft line. The FC sensor collector plate is divided into two, semi-circular halves; the division line is parallel to the spacecraft spin plane which is approximately parallel to the ecliptic plane. The split collector allow determination of the bulk plasma flow relative to the spin plane; North/South angles refer to flows coming from above or below the spin plane respectively (flows from the South are designated as having a positive N/S angle). The bulk flow angle in the spin plane is determined from the measurements of current vs. rotation angle. The currents telemetered to the ground are the sums of currents for the two half-collectors ("A" and "B") and, for the TMS and AQM modes, also the current for the half-collector "B". Electrons are measured except for the eight angles near the Sun. The experiment has two memories only one of which is operating perfectly. As a result, only every other TMS spectrum is usable, and the time between spectra is usually twice that that would be expected from the spacecraft spin rate. The bad half-memory also limits the energy windows that can be used in the other modes, since they require both memories to hold the data. On occasion, the data are read out rapidly enough by the spacecraft to allow repeated use of the good half-memory, and the time resolution in the TMS is approximately 32 seconds. |

14) | IMP 8 MAG PLS 1-min field and plasma data at bow shock nose | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/IMP8/Propagated/PT1M | ||||||||||||||||||

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Solar wind magnetic field and plasma data at 1-min resolution created from IMP 8 data shifted to the Earth's bow shock nose (BSN). |

15) | IMP-8 Linearly Interpolated 60 s Resolution Tri-axial Fluxgate Magnetometer in GSE Coordinates | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Weygand/IMP8/MAG/Processed/GSE/PT60S | ||||||||||||||||||

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IMP-8 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) | IMP-8 Linearly Interpolated 60 s Resolution Tri-axial Fluxgate Magnetometer in GSM Coordinates | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Weygand/IMP8/MAG/Processed/GSM/PT60S | ||||||||||||||||||

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IMP-8 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) | IMP-8 Weimer Propagated 60 s Resolution Tri-axial Fluxgate Magnetometer in GSE Coordinates | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Weygand/IMP8/MAG/Propagated.PLS/GSE/PT60S | ||||||||||||||||||

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IMP-8 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) | IMP-8 Weimer Propagated 60 s Resolution Tri-axial Fluxgate Magnetometer in GSM Coordinates | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Weygand/IMP8/MAG/Propagated.PLS/GSM/PT60S | ||||||||||||||||||

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IMP-8 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) | IMP-8 Linearly Interpolated 60 s Resolution PLS data in GSE Coordinates | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Weygand/IMP8/PLS/Processed/GSE/PT60S | ||||||||||||||||||

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IMP-8 linearly interpolated to have the measurements on the minute at 60 s resolution PLS 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. |

20) | IMP-8 Linearly Interpolated 60 s Resolution PLS data in GSM Coordinates | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Weygand/IMP8/PLS/Processed/GSM/PT60S | ||||||||||||||||||

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IMP-8 linearly interpolated to have the measurements on the minute at 60 s resolution PLS 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. |

21) | IMP-8 PLS Solar Wind Weimer Propagated 60 s Resolution Data in GSE Coordinates | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Weygand/IMP8/PLS/Propagated.PLS/GSE/PT60S | ||||||||||||||||||

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IMP-8 PLS propagated solar wind data and linearly interpolated to have the measurements on the minute at 60 s resolution data in GSE coordinates. This data set consists of propagated solar wind data that has first been propagated to a position just outside of the nominal bow shock (about 17, 0, 0 Re) and then linearly interpolated to 1 min resolution using the interp1.m function in MATLAB. The input data for this data set is a 1 min resolution processed solar wind data constructed by Dr. J.M. Weygand. The method of propagation is similar to the minimum variance technique and is outlined in Dan Weimer et al. [2003; 2004]. The basic method is to find the minimum variance direction of the magnetic field in the plane orthogonal to the mean magnetic field direction. This minimum variance direction is then dotted with the difference between final position vector minus the original position vector and the quantity is divided by the minimum variance dotted with the solar wind velocity vector, which gives the propagation time. This method does not work well for shocks and minimum variance directions with tilts greater than 70 degrees of the sun-earth line. This data set was originally constructed by Dr. J.M. Weygand for Prof. R.L. McPherron, who was the principle investigator of two National Science Foundation studies: GEM Grant ATM 02-1798 and a Space Weather Grant ATM 02-08501. These data were primarily used in superposed epoch studies References: Weimer, D. R. (2004), Correction to ??Predicting interplanetary magnetic field (IMF) propagation delay times using the minimum variance technique,?? J. Geophys. Res., 109, A12104, doi:10.1029/2004JA010691. Weimer, D.R., D.M. Ober, N.C. Maynard, M.R. Collier, D.J. McComas, N.F. Ness, C. W. Smith, and J. Watermann (2003), Predicting interplanetary magnetic field (IMF) propagation delay times using the minimum variance technique, J. Geophys. Res., 108, 1026, doi:10.1029/2002JA009405. |

22) | IMP-8 PLS Solar Wind Weimer Propagated 60 s Resolution Data in GSM Coordinates | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Weygand/IMP8/PLS/Propagated.PLS/GSM/PT60S | ||||||||||||||||||

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IMP-8 PLS Weimer propagated solar wind data and linearly interpolated to have the measurements on the minute at 60 s resolution 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. |

23) | IMP-8 Weimer Propagation Details at 1 min Resolution | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Weygand/IMP8/TAP/Propagated.PLS/GSE/PT60S | ||||||||||||||||||

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IMP-8 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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