Showing 1 - 40 |

1) | AMPTE/IRM Plasma Data | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/AMPTE_IRM/Plasma/PT4.4S | ||||||||||||||||||

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AMPTE/IRM spin-averaged plasma moments at ~4.4 second resolution. |

2) | Geotail 1-min magnetic field and plasma data, solar wind only | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/Geotail/CPI-MGF/PT1M | ||||||||||||||||||

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Geotail 1-min-averaged magnetic field and plasma parameter data. Field data include GSE and GSM cartesian components and standard deviations in the averages. Plasma data include flow speed, density, temperature and GSE flow velocity components. Non-fill data are nominally from the solar wind only. Geotail location information is included. Data are in ASCII. |

3) | Geotail CPI Hot Plasma Moments | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Geotail/CPI/HPA_PT64S | ||||||||||||||||||

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The CPI/HPA Hot Plasma Analyzer high time resolution moments of hot plasma: * Ion number density * Ion average temperature * Ion bulk flow velocity * Electron number density * Electron average temperature The CPI/HPA data are good in the magnetosphere and may be usefull in the magnetosheath. |

4) | Geotail CPI Definitive Solar Wind Moments | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Geotail/CPI/SWA_PT48S | ||||||||||||||||||

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The CPI Solar Wind analyzer definitive plasma moments. The CPI/SW data are good in the solar wind and may be usefull in the magnetosheath. |

5) | Geotail Comprehensive Plasma Instrumentation (CPI) Hot Plasma Analyzer high Res data at 64 s resolution in GSE Coordinates | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Geotail/CPI/UIOWA_HPA_PT64S | ||||||||||||||||||

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Geotail Comprehensive Plasma Instrumentation (CPI) Hot Plasma Analyzer data in GSE coordinates. This data set consists of plasma flow vectors, density, and temperature data. |

6) | Geotail Comprehensive Plasma Instrumentation (CPI) data at 48 s resolution in GSE Coordinates | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Geotail/CPI/UIOWA_PT48S | ||||||||||||||||||

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Geotail Comprehensive Plasma Instrumentation (CPI) data in GSE coordinates. This data set consists of solar wind flow vectors, density, and temperature data. |

7) | Geotail CPI Plasma Key Parameters (64s) | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Geotail/CPI/kp_PT64S | ||||||||||||||||||

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A combination of plasma key parameters from the Geotail CPI analyzers. The CPI-SW Solar Wind Analyzer provides * Ion number density * Average proton energy * Bulk flow velocity The CPI-HP Hot Plasma Analyzer provides * Ion number density * Average proton energy * Average electron energy * Bulk flow velocity * Plasma pressure The CPI-IC Ion Composition Analyzer provides principal Species * H+ * He++ * He+ * O+ |

8) | Geotail EPIC Summary Plots | |||||||||||||||||
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Resource ID:spase://VSPO/DisplayData/Geotail/EPIC/PLOTS | ||||||||||||||||||

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GIF plots, several types per 12-hr interval |

9) | Geotail EPIC 96-sec Key Parameters | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/Geotail/EPIC/PT96S | ||||||||||||||||||

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Geotail EPIC (Energetic Particles & Ion Composition) 96-sec Key Parameters |

10) | Geotail Editor-A 12 second Low-Energy Particles | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Geotail/LEP/EDA.PT12S | ||||||||||||||||||

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12-second Editor-A low-energy particle data from the Geotail spacecraft. Editor-A data are only acquired with the real-time operation in Usuda Deep Space Center (UDSC),Japan, while the Editor-B data are 24-hours continuouslyrecorded in the onboard tape recorders and are dumpedover the NASA/JPL Deep Space Network (DSN) stations. The ion energy analyzer (LEP-EAi) has two energy scan mode: RAM-A (60 eV to 40 keV) and RAM-B (5 keV to 40 keV). RAM-B is selected to protect the very sensitive detector from intense low energy fluxes that are usually seen in the solar wind and magnetosheath. The energy scan mode is automatically selected onboard depending on incoming ion fluxes. At present, only the ion moments in the RAM-A mode are listed for the LEP-EAi data. The ion moment data of the solar wind analyzer (LEP-SW) should be used only qualitatively. The LEP-SW ion moments are listed when the energy scan mode of LEP-EAi is RAM-B. |

11) | Geotail Editor-B 12 second Low-Energy Particles | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Geotail/LEP/EDB.PT12S | ||||||||||||||||||

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12-second Editor-B low-energy particle data from the Geotail spacecraft. Editor-A data are only acquired with the real-time operation in Usuda Deep Space Center (UDSC),Japan, while the Editor-B data are 24-hours continuouslyrecorded in the onboard tape recorders and are dumpedover the NASA/JPL Deep Space Network (DSN) stations. The ion energy analyzer (LEP-EAi) has two energy scan mode: RAM-A (60 eV to 40 keV) and RAM-B (5 keV to 40 keV). RAM-B is selected to protect the very sensitive detector from intense low energy fluxes that are usually seen in the solar wind and magnetosheath. The energy scan mode is automatically selected onboard depending on incoming ion fluxes. At present, only the ion moments in the RAM-A mode are listed for the LEP-EAi data. The ion moment data of the solar wind analyzer (LEP-SW) should be used only qualitatively. The LEP-SW ion moments are listed when the energy scan mode of LEP-EAi is RAM-B. |

12) | Geotail LEP 64-sec Key Parameters | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/Geotail/LEP/PT64S | ||||||||||||||||||

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Geotail LEP (Low-Energy Particles) 64-sec Solar Wind Key Parameters |

13) | Interball Tail Plasma Electron 2-min Key Parameters | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/Interball-1/ELECTRON/PT120S | ||||||||||||||||||

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Interball Tail ELECTRON Plasma Electron 2-min Key Parameters (Density and Mean Energy) |

14) | Pioneer 10 Hourly Plasma Version 3.1 Data | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/Pioneer10/PLS/PT1H | ||||||||||||||||||

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This data set contains Version 3.1 final archival set of hourly averaged solar wind data from the Plasma Analyzer of the Pioneer 10 mission. It includes plasma bulk parameters in ASCII format: bulk velocity, proton number density, proton temperature, and flow angles. This is the same data set as NSSDC ID SPHE-00066 or 72-012A-13L, which is in binary format. |

15) | Pioneer 10 full resolution plasma data | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/Pioneer10/PLS/PT600.00S | ||||||||||||||||||

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Pioneer 10 plasma ion density, temperature, flow speed and direction angles, full resolution (10 minutes or lower resolution) |

16) | Pioneer 11 Plasma 1-hr data | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/Pioneer11/PLS/PT60M | ||||||||||||||||||

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This data set consists of hourly resolution data in ASCII format from the Pioneer 11 Plasma Analyzer. It contains five types of data: 'REDR' and EDR data, Spectral' data, 'summary' (high resolution) parameter data, hourly averaged parameter data, and trajectory data. The plasma bulk parameters (bulk velocity, proton number density, proton temperature, and flow angles) were obtained using one of three processing schemes described in the data set documentation. Hourly averaged data files were created by averaging every valid parameter in each hour, regardless of the processing scheme used to derive it. Each plasma data file contains a header followed by data records. The filename format is p10_XX_YYh.asc where XX and YY are the start and end years of data in the file. Each data record contains the spacecraft ID (SCID), year, day of year, and time of day in hours, followed by the bulk velocity, number density, temperature, and where appropriate, the flow angles. Speeds are given in km/s, number densities are given in #/cc, temperatures are given in K, and flow angles are given in degrees. Prior to day Jan. 31, 1989, all directions are given in a spacecraft-centered ecliptic system, in which the E/W angle is positive in the direction of planetary rotation while a N/S angle of zero means that the solar wind flow is parallel to the plane of the ecliptic. After Jan. 31, 1989 the flow directions are given with respect to a RTN heliographic system for which the R component is radially outward from the Sun, T is in the direction of planetary orbital motion around the Sun, and N is orthogonal (RxT) to R and T. |

17) | Geotail Linearly Interpolated 60 s Resolution Coordinates Comprehensive Plasma Instrumentation (CPI) data in GSE | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Weygand/Geotail/CPI/Processed/GSE/PT60S | ||||||||||||||||||

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Geotail linearly interpolated to have the measurements on the minute at 60 s resolution CPI 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. |

18) | Geotail Linearly Interpolated 60 s Resolution Coordinates Comprehensive Plasma Instrumentation (CPI) data in GSM | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Weygand/Geotail/CPI/Processed/GSM/PT60S | ||||||||||||||||||

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Geotail linearly interpolated to have the measurements on the minute at 60 s resolution CPI 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. |

19) | Geotail Comprehensive Plasma Instrumentation (CPI) data Weimer Propagated 60 s Resolution in GSE Coordinates | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Weygand/Geotail/CPI/Propagated.CPI/GSE/PT60S | ||||||||||||||||||

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Geotail Weimer propagated solar wind data and linearly interpolated to have the measurements on the minute at 60 s resolution CPI 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. |

20) | Geotail Comprehensive Plasma Instrumentation (CPI) data Weimer Propagated 60 s Resolution in GSM Coordinates | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Weygand/Geotail/CPI/Propagated.CPI/GSM/PT60S | ||||||||||||||||||

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Geotail Weimer propagated solar wind data and linearly interpolated to have the measurements on the minute at 60 s resolution CPI 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. |

21) | Geotail Linearly Interpolated 60 s Resolution Low Energy Particle (LEP) experiment data in GSE Coordinates | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Weygand/Geotail/LEP/Processed/GSE/PT60S | ||||||||||||||||||

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Geotail linearly interpolated to have the measurements on the minute at 60 s resolution LEP 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. |

22) | Geotail Linearly Interpolated 60 s Resolution Low Energy Particle (LEP) experiment data in GSM Coordinates | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Weygand/Geotail/LEP/Processed/GSM/PT60S | ||||||||||||||||||

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Geotail linearly interpolated to have the measurements on the minute at 60 s resolution LEP 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. |

23) | Geotail Low Energy Particle (LEP) experiment data Weimer Propagated 60 s Resolution in GSE Coordinates | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Weygand/Geotail/LEP/Propagated.LEP/GSE/PT60S | ||||||||||||||||||

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Geotail LEP 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. |

24) | Geotail Low Energy Particle (LEP) experiment data Weimer Propagated 60 s Resolution in GSM Coordinates | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Weygand/Geotail/LEP/Propagated.LEP/GSM/PT60S | ||||||||||||||||||

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Geotail LEP 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. |

25) | Geotail Solar Wind Weimer Propagation Details at 1 min Resolution | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Weygand/Geotail/TAP/Propagated.CPI/GSE/PT60S | ||||||||||||||||||

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

26) | Wind 3DP Linearly Interpolated 60 s Resolution data in GSE Coordinates | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Weygand/Wind/3DP/Processed/GSE/PT60S | ||||||||||||||||||

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Wind linearly interpolated to have the measurements on the minute at 60 s resolution 3DP 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. |

27) | Wind 3DP Linearly Interpolated 60 s Resolution data in GSM Coordinates | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Weygand/Wind/3DP/Processed/GSM/PT60S | ||||||||||||||||||

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Wind linearly interpolated to have the measurements on the minute at 60 s resolution 3DP 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. |

28) | Wind 3DP Weimer Propagated 60 s Resolution in GSE Coordinates | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Weygand/Wind/3DP/Propagated.3DP/GSE/PT60S | ||||||||||||||||||

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Wind 3DP 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. There are now two version of this data set. An off set has been found in the Wind MFI Bz component that is present after November 2004. Version 2 has this offset removed. Prof. R.L. McPherron determined the correction to be Bz = Bz - (-0.000000130406219.*odoy.*odoy + 0.000576303146.*odoy + 0.679940509 + 0.3215*cos(2*pi*(doy-171)/366)) where doy is the day of the year in units of days and odoy is the days sinces Jan 1, 1999 00:00:00 UT in units of days. |

29) | Wind 3DP Weimer Propagated 60 s Resolution in GSM Coordinates | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Weygand/Wind/3DP/Propagated.3DP/GSM/PT60S | ||||||||||||||||||

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Wind 3DP 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. There are now two version of this data set. An off set has been found in the Wind MFI Bz component that is present after November 2004. Version 2 has this offset removed. Prof. R.L. McPherron determined the correction to be Bz = Bz - (-0.000000130406219.*odoy.*odoy + 0.000576303146.*odoy + 0.679940509 + 0.3215*cos(2*pi*(doy-171)/366)) where doy is the day of the year in units of days and odoy is the days sinces Jan 1, 1999 00:00:00 UT in units of days. |

30) | Wind 3DP EESA-HIGH Electron Pitch Angle Distributions | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/Wind/3DP/EESA_HIGH/PD/PT24S | ||||||||||||||||||

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Wind 3DP electron pitch angle product providing electron fluxes in 8 directional bins relative to the local magnetic field direction at 15 different energy levels. |

31) | Wind 3DP 24-sec ESSA-HIGH Electron Omnidirectional Fluxes | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/Wind/3DP/EESA_HIGH/SP/PT24S | ||||||||||||||||||

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Electron omnidirectional fluxes 100 eV-30 keV, often at 24 sec, EESA High, Wind 3DP - R. Lin (UC Berkeley) |

32) | Wind 3DP EESA-LOW Electron Moments | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/Wind/3DP/EESA_LOW/Moments | ||||||||||||||||||

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Electron Moments (ground-computed), EESA Low, Wind 3DP - R. Lin (UC Berkeley) |

33) | Wind 3DP 24-sec ESSA LOW Electron Omnidirectional Fluxes | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/Wind/3DP/EESA_LOW/SP/PT24S | ||||||||||||||||||

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This set of plasma data in the interplanetary medium was derived from the Wind 3-D Plasma and Energetic Particle Experiment, specifically from the electron electrostatic analyzers LOW (EESA LOW) measurements of electron fluxes in omnidirections from 3 eV to 30 keV. |

34) | Wind 3DP Electron Plasma Moments | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/Wind/3DP/EM/PT3S | ||||||||||||||||||

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Electron Plasma moments (computed on-board) (NOT CORRECTED FOR S/C POTENTIAL) @ 3 second (spin) resolution (version 3), EESA LOW, Wind 3DP - R. Lin (UC Berkeley) |

35) | Wind 3DP 92-s Key Parameters | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/Wind/3DP/KeyParameters/PT92S | ||||||||||||||||||

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Wind 3DP (3-D Plasma Analyzer), 92-s key parameters, ion and electron fluxes (at 7 energy steps), flow velocities, densities and temperatures |

36) | Wind 3DP SST Foil Electron Energy-Angle Distributions | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/Wind/3DP/SST_Foil/PD/PT24S | ||||||||||||||||||

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Electron energy-angle distributions 27-520 keV, often at 24 sec, SST Foil, Wind 3DP - R. Lin (UC Berkeley) |

37) | Wind 3DP SST Foil Electron Omnidirectional Fluxes | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/Wind/3DP/SST_Foil/SP/PT24S | ||||||||||||||||||

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Electron omnidirectional fluxes 27-520 keV, often at 24 sec, SST Foil, Wind 3DP - R. Lin (UC Berkeley) |

38) | Wind 3DP SST Open Proton Energy-Angle Distributions | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/Wind/3DP/SST_Open/PD/PT24S | ||||||||||||||||||

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Proton energy-angle distributions 70 keV - 6.8 MeV, often at 24 sec, SST Open, Wind 3DP - R. Lin (UC Berkeley) |

39) | Wind 3DP SST Open Proton Omniderectional Fluxes | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/Wind/3DP/SST_Open/SP/PT24S | ||||||||||||||||||

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Proton omnidirectional fluxes 70 keV - 6.8 MeV, often at 24 sec, SST Open, Wind 3DP - R. Lin (UC Berkeley) |

40) | Wind 3DP Plasma data at UCB | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/Wind/3DP/UCB/PT24.00S | ||||||||||||||||||

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Wind 3DP thermal and energetic ion and electron distributions and moments, multiple CDF file types |

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