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1) | Geotail PWI 64-sec Key Parameters | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/GEOTAIL/PWI/KP/PT64S | ||||||||||||||||||

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This set of key paraments from the Geotail Plasma Wave Instrument includes: Peak and average electric and magnetic spectra from the multichannel analyzer MCA (at 5 frequencies from 5.6 Hz to 311 kHz for the electric antenna and at 4 frequencies from 5.6 Hz to 10 kHz for the magnetic coils); Peak and average spectra intentsities (scala only) averaged over 64 seconds from the Sweep Frequency Analyzer SFA (24 Hz to 800 kHz); Frequency corresponding to the peak of the spectral intensities (scalar only); and spacecraft position in GSE cartesian coordinates. |

2) | Geotail field and plasma data propagated to (17,0,0) Re | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/Geotail/CPI-MGF-LEP/PT1M | ||||||||||||||||||

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This is a family of data sets containing 1-min resolution Geotail magnetic field and plasma parameters, in GSE and GSM coordinates, both at the location of the Geotail spacecraft and as propagated to the location (17,0,0) Re, GSE. Plasma data are from both the CPI and LEP plasma instruments, while field data are from the MGF instrument. Parallel groups of CPI-based and LEP-based data sets are available for the full Geotail mission. Data taken when the spacecraft was inside the Spreiter et al (1966) model bow shock were excluded. Propagation was done by J. Weygand using software provided by D. Weimer. The software determines normal directions to assumed planar phase fronts using a modified minimum variance analysis of 1-min magnetic field data, and propagates data using these normals and the Wind-observed solar wind flow velocity. Magnetic field data consist of three Cartesian components, while plasma data consist of three Cartesian components of the flow velocity vector plus proton density and temperature. Data are current to within about 3 months. Different subdirectories hold data for unique combinations of field vs. plasma parameters, GSE vs. GSM coordinates, CPI-based vs. LEP-based data, and propagated vs. unpropagated data. See the VMO interface for a more detailed breakout. |

3) | 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. |

4) | 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. |

5) | 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. |

6) | 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. |

7) | 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. |

8) | 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+ |

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

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Geotail EFD (Electric Field Detector) 64-sec Key Parameters |

10) | 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 |

11) | 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 |

12) | Geotail Definitive Attitude | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/Geotail/Ephemeris/Def_AT/PT10M | ||||||||||||||||||

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Definitive Geotail spacecraft attitude in various coordinate systems. |

13) | Geotail Spacecraft Definitive Positions | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Geotail/Ephemeris/PT10M | ||||||||||||||||||

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Definitive Geotail spacecraft positions in various coordinate systems |

14) | Geotail Predicted Orbit | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/Geotail/Ephemeris/PT600S | ||||||||||||||||||

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Geotail Predicted Orbit at 10-min Resolution |

15) | Geotail Predicted Attitude | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/Geotail/Ephemeris/Pre_AT/PT10M | ||||||||||||||||||

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Predicted Geotail spacecraft attitude in various coordinate systems. |

16) | Geotail Spin Phase Key Parameters | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/Geotail/Ephemeris/Spin_Phase_KP/PT10M | ||||||||||||||||||

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This data set contains selected Key Parameters of the spin phase angle information for the Geotail spacecraft: the spacecraft spin phase angle, spin rate, and a fault flag are given versus time. |

17) | Geotail Daily Survey Plots | |||||||||||||||||
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Resource ID:spase://VSPO/DisplayData/Geotail/GWS | ||||||||||||||||||

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Daily gif_walk plots, selected data from many Geotail instruments |

18) | 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. |

19) | 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. |

20) | 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 |

21) | Geotail Editor-A 3-second Magnetic Field Data | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Geotail/MGF/EDA.PT3S | ||||||||||||||||||

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3-second Editor-A magnetic field data from the Geotail spacecraft. As of February 1 2008 the Bz component of the magnetic field has been corrected in the data set. The Geotail satellite has two editors onboard: The Editor-A data are only acquired with the real-time operation in Usuda Deep Space Center (UDSC) or Uchinoura Space Center (USC), Japan, while the Editor-B data are continuously recorded in the onboard tape recorders for 24 hours and are dumped to the NASA JPL Deep Space Network (DSN) stations. |

22) | Geotail Editor-B 3-second Magnetic Field Data | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Geotail/MGF/EDB.PT3S | ||||||||||||||||||

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3-second Editor-B magnetic field data from the Geotail spacecraft. As of February 1 2008 the Bz component of the magnetic field has been corrected in the data set. The Geotail satellite has two editors onboard: The Editor-A data are only acquired with the real-time operation in Usuda Deep Space Center (UDSC) or Uchinoura Space Center (USC), Japan, while the Editor-B data are continuously recorded in the onboard tape recorders for 24 hours and are dumped to the NASA JPL Deep Space Network (DSN) stations. |

23) | Geotail 15-sec magnetic field data, solar wind only | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Geotail/MGF/PT15S | ||||||||||||||||||

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Data consist of 15-sec averages of magnetic field magnitude and GSE Cartesian components, from the MGF magnetometer on Geotail. Data are for only the solar wind phases of the Geotail orbit. The Geotail position vector in GSE coordinates is included. |

24) | Geotail 3-sec magnetic field data | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/Geotail/MGF/PT3.00S | ||||||||||||||||||

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Geotail 3-sec magnetic field data from ISAS/DARTS |

25) | Geotail KP Magnetic Field Data (64s) | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Geotail/MGF/PT64S | ||||||||||||||||||

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This data set contains the investigator-selected Key Parameters from the Magnetic Field instrument (MGF) on Geotail, as made available via NSSDC's interactive WWW interface CDAWeb. Selected references: Kokubun, S., et al., Magnetic field measurement (MGF), In Geotail Prelaunch Report, SES-TD-92-007SY, Institute of Space and Astronautical Science, SES Data Center, pp. 58-70, Apr. 1992. Nishida, A., et al., Geotail mission to explore earth's magnetotail, EOS, 73, No. 40, Oct. 1992. Kokubun, S., et al., The GEOTAIL Magnetic Field Experiment, J. Geomag. Geoelectr., 46, No. 1, 7-21, 1994. |

26) | Geotail PWI 24 hour dynamic spectrograms | |||||||||||||||||
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Resource ID:spase://VWO/DisplayData/Geotail/PWI/DS.P1D | ||||||||||||||||||

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Geotail PWI SFA and MCA dynamic spectrogram plots with frequency in Hz on the vertical axis and time in UT on the horizontal axis. Each file contains one spectrogram from the electric field antennas and one from the magnetic field search coils. The electric field spectrograms span the frequency range 5.62 to 24 Hz (the Multi-Channel Analyzer - MCA instrument) and 24 Hz to 800 kHz (the Sweep Frequency Analyzer - SFA instrument). The intensity values are color coded and are expressed in units of dBV/m/root-Hz. The magnetic field spectrograms also combine the MCA and SFA instruments and span the frequency range 5.62 Hz to 12.5 kHz. The intensity values are color coded and are expressed in units of dB nT/root-Hz. Each plot spans 24 hours. Beneath the time axis of the magnetic field spectrogram are spacecraft GSM coordinates for every 4 hours. Information on the instrument and antenna status is also provided above each spectrogram. |

27) | Geotail PWI 2 hour dynamic spectrograms | |||||||||||||||||
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Resource ID:spase://VWO/DisplayData/Geotail/PWI/DS.PT2H | ||||||||||||||||||

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Geotail PWI SFA and MCA dynamic spectrogram plots with frequency in Hz on the vertical axis and time in UT on the horizontal axis. Each file contains one spectrogram from the electric field antennas and one from the magnetic field search coils. The electric field spectrograms span the frequency range 5.62 to 24 Hz (the Multi-Channel Analyzer - MCA instrument) and 24 Hz to 800 kHz (the Sweep Frequency Analyzer - SFA instrument). The intensity values are color coded and are expressed in units of dBV/m/root-Hz. The magnetic field spectrograms also combine the MCA and SFA instruments and span the frequency range 5.62 Hz to 12.5 kHz. The intensity values are color coded and are expressed in units of dB nT/root-Hz. Each plot spans 2 hours. Information on the instrument and antenna status is also provided above each spectrogram. |

28) | Geotail MGF CPI 1-min field and plasma data at bow shock nose | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Geotail/Propagated/PT1M | ||||||||||||||||||

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

29) | 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. |

30) | 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. |

31) | 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. |

32) | 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. |

33) | 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. |

34) | 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. |

35) | 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. |

36) | 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. |

37) | Geotail Linearly Interpolated 60 s Resolution Tri-axial Fluxgate Magnetometer in GSE Coordinates | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Weygand/Geotail/MGF/Processed/GSE/PT60S | ||||||||||||||||||

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Geotail 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. |

38) | Geotail Linearly Interpolated 60 s Resolution Tri-axial Fluxgate Magnetometer in GSM Coordinates | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Weygand/Geotail/MGF/Processed/GSM/PT60S | ||||||||||||||||||

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Geotail 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. |

39) | Geotail Weimer Propagated using CPI 60 s Resolution Tri-axial Fluxgate Magnetometer in GSM Coordinates | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Weygand/Geotail/MGF/Propagated.CPI/GSE/PT60S | ||||||||||||||||||

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Geotail Weimer propagated solar wind data using CPI 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. |

40) | Geotail Weimer Propagated using CPI 60 s Resolution Tri-axial Fluxgate Magnetometer in GSM Coordinates | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Weygand/Geotail/MGF/Propagated.CPI/GSM/PT60S | ||||||||||||||||||

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Geotail Weimer propagated solar wind data using CPI 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. |

41) | Geotail Weimer Propagated using LEP 60 s Resolution Tri-axial Fluxgate Magnetometer in GSE Coordinates | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Weygand/Geotail/MGF/Propagated.LEP/GSE/PT60S | ||||||||||||||||||

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Geotail Weimer propagated solar wind data using LEP 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. |

42) | Geotail Weimer Propagated using LEP 60 s Resolution Tri-axial Fluxgate Magnetometer in GSM Coordinates | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Weygand/Geotail/MGF/Propagated.LEP/GSM/PT60S | ||||||||||||||||||

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Geotail Weimer propagated solar wind data using LEP 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. |

43) | 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. |

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