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1) | 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. |

2) | 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. |

3) | 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. |

4) | 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. |

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

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Wind 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. 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. |

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

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Wind 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. 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. |

7) | Wind Weimer Propagated 60 s Resolution Tri-axial Fluxgate Magnetometer in GSE Coordinates | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Weygand/Wind/MFI/Propagated.3DP/GSE/PT60S | ||||||||||||||||||

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Wind 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. 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. |

8) | Wind Weimer Propagated 60 s Resolution Tri-axial Fluxgate Magnetometer in GSM Coordinates | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Weygand/Wind/MFI/Propagated.3DP/GSM/PT60S | ||||||||||||||||||

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Wind 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. 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. |

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

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

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

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

11) | Wind SWE Weimer Propagated 60 s Resolution data in GSE Coordinates | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Weygand/Wind/SWE/Propagated.SWE/GSE/PT60S | ||||||||||||||||||

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Wind SWE 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. |

12) | Wind SWE Weimer Propagated 60 s Resolution data in GSM Coordinates | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Weygand/Wind/SWE/Propagated.SWE/GSM/PT60S | ||||||||||||||||||

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Wind SWE 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. |

13) | Wind Solar Wind Weimer Propagation Details at 1 min Resolution | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Weygand/Wind/TAP/Propagated.3DP/GSE/PT60S | ||||||||||||||||||

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Wind 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. |

14) | Wind EPACT/LEMT 1-Hr H,He,O,Fe Anisotropies for Events | |||||||||||||||||
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Resource ID:spase://VEPO/NumericalData/Wind/EPACT/LEMT/Events/A1S/PT1H | ||||||||||||||||||

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This data set contains hourly resolution anisotropies in spacecraft and solar wind frames for 2.5-5 MeV/n H, He, O and Fe nuclei, plus 5-8 MeV/n He nuclei. First-, second- and third-order spacecraft-frame anisotropies, and the magnitude and direction angles, relative to the mean magnetic field, of the spacecraft-frame first-order anisotropy vectors are given. Ion spectral parameters used in anisotropy determinations, namely spectral power law index (gamma), mean energy of ions in sampled energy range, and ion flux at the mean energy, are given. Many solar wind parameter averages are given, including magnetic field magnitude and direction, solar wind density and flow speed and azimuthal angle. Standard deviations in all hourly averages are also given. See Tan et al, Ap.J.,661, 1297-1310, 2007, for discussions of anisotropies, reference frames, etc. As of 10/2011, the data cover 39 1997-2006 multi- day intervals that include energetic solar particle events. ASCII data words are comma-separated. For a given particle event, there are species-specific files. File naming uses the convention XX_a1s_YYYYMMDD, where XX = H (or Hng), He2 (2.5-5 MeV/n), He5 (5-8 MeV/n), O or Fe, and where YYYYMMDD is the day of the first record of the file. "Hng" means hydrogen - no gamma (as obtained from IMP 8 GME data); but see the readme file cited below on the use of EPACT/LEMT He data as providing an alternative power law index. |

15) | Wind EPACT/LEMT 1-Hr Omnidirectional Fluxes | |||||||||||||||||
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Resource ID:spase://VEPO/NumericalData/Wind/EPACT/LEMT/Events/OMNI/PT1H | ||||||||||||||||||

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This dataset contains hourly-averaged omnidirectional fluxes for He, C, O, Ne, Si, and Fe in particles/cm2-sr-s-MeV/nuc in seven energy bins (six for Ne) in the general range of 2-10 MeV/nucleon. The error bars are statistical only, that is, corresponding to sqrt(N), where N is the number of collected ions. For intervals in which zero ions were observed, the error bar corresponds to one ion. ASCII listing generated from this link provide the start-time of the averaging interval as YYYY DD HH, followed by pairs of numbers giving the flux and its uncertainty from the selected intervals. The available energy bins for the species are He: 2.00-2.40, 2.40-3.00, 3.00-3.70, 3.70-4.53, 4.53-6.00, 6.00-7.40, 7.40-9.64 MeV/nuc C: 2.57-3.19, 3.19-3.85, 3.85-4.80, 4.80-5.80, 5.80-7.20, 7.20-9.10, 9.10-13.70 MeV/nuc O: 2.56-3.17, 3.17-3.88, 3.88-4.68, 4.68-6.00, 6.00-7.40, 7.40-9.20, 9.20-13.40 MeV/nuc Ne: 3.27-3.98, 3.98-4.72, 4.72-5.92, 5.92-7.87, 7.87-9.96, 9.96-12.7 MeV/nuc Si: 2.50-3.20, 3.20-4.00, 4.00-4.90, 4.90-6.00, 6.00-7.90, 7.90-9.70, 9.70-13.60 MeV/nuc Fe: 2.40-3.00, 3.00-3.95, 3.95-4.80, 4.80-5.90, 5.90-7.80, 7.80-9.30, 9.30-12.50 MeV/nuc |

16) | Wind EPACT/LEMT 5-min Omnidirectional Fluxes | |||||||||||||||||
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Resource ID:spase://VEPO/NumericalData/Wind/EPACT/LEMT/Events/OMNI/PT5M | ||||||||||||||||||

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This dataset contains 5-min omnidirectional fluxes for He, C, O, Ne, Si, and Fe in particles/cm2-sr-s-MeV/nuc in seven energy bins (six for Ne) in the general range of 2-10 MeV/nucleon. The error bars are statistical only, that is, corresponding to sqrt(N), where N is the number of collected ions. For intervals in which zero ions were observed, the error bar corresponds to one ion. ASCII listing generated from this link provide the start-time of the averaging interval as YYYY DD HH, followed by pairs of numbers giving the flux and its uncertainty from the selected intervals. The available energy bins for the species are He: 2.00-2.40, 2.40-3.00, 3.00-3.70, 3.70-4.53, 4.53-6.00, 6.00-7.40, 7.40-9.64 MeV/nuc C: 2.57-3.19, 3.19-3.85, 3.85-4.80, 4.80-5.80, 5.80-7.20, 7.20-9.10, 9.10-13.70 MeV/nuc O: 2.56-3.17, 3.17-3.88, 3.88-4.68, 4.68-6.00, 6.00-7.40, 7.40-9.20, 9.20-13.40 MeV/nuc Ne: 3.27-3.98, 3.98-4.72, 4.72-5.92, 5.92-7.87, 7.87-9.96, 9.96-12.7 MeV/nuc Si: 2.50-3.20, 3.20-4.00, 4.00-4.90, 4.90-6.00, 6.00-7.90, 7.90-9.70, 9.70-13.60 MeV/nuc Fe: 2.40-3.00, 3.00-3.95, 3.95-4.80, 4.80-5.90, 5.90-7.80, 7.80-9.30, 9.30-12.50 MeV/nuc |

17) | Wind EPACT/LEMT 1-Hr Spin-Sectored H,He,O,Fe Counts for Events | |||||||||||||||||
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Resource ID:spase://VEPO/NumericalData/Wind/EPACT/LEMT/Events/SEC/PT1H | ||||||||||||||||||

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This data set contains hourly counts of H, He, O and Fe nuclei in 16 look directions about the spacecraft spin axis. Counts for each of the four species are given at 2.5-5 MeV/n, and an additional count is given for 5-8 MeV/n He. As of 10/2011, the data cover 39 1997-2006 multi-day intervals that include energetic solar particle events. ASCII data words are comma-separated. For a given particle event, there are species-specific files. File naming uses the convention XX_sec_YYYYMMDD, where XX = H, He2 (2.5-5 MeV/n), He5 (5-8 MeV/n), O or Fe, and where YYYYMMDD is the day of the first record of the file. Sectoring is defined with respect to the ecliptic plane projection of the concurrently measured magnetic field vector. The edge of sector #1 is coincided with the projection of B on the ecliptic plane, so phi value of the center of sector i is phiB+11.25+(i-1)*22.5 deg, where phiB is the longitudinal angle of B. |

18) | Wind EPACT 92s KP Fluxes | |||||||||||||||||
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Resource ID:spase://VEPO/NumericalData/Wind/EPACT/PT92S | ||||||||||||||||||

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This set of key parameter flux data from the Wind EPACT (Energetic Particles: Acceleration, Composition and Transport) telescopes contains fluxes of protons (19-72 MeV in 2 energy bins), He nuclei (0.08-72 MeV/n in 5 bins), CNO nuclei (80-640 MeV/n in 2 bins), O nuclei (3.2-6.2 MeV/n in 1 bin), Fe nuclei (0.08-6.2 MeV/n in 3 bins) and 1-10 MeV electrons, each averaged over 92 seconds. |

19) | Wind WAVES All Instruments Daily Summary Color Dynamic Spectrograms | |||||||||||||||||
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Resource ID:spase://VWO/DisplayData/Wind/WAVES/All/DS.Color.PS.P1D | ||||||||||||||||||

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Wind Waves RAD2, RAD1, and TNR dynamic spectrogram plots with frequency in kHz on the vertical axis and time in UT on the horizontal axis. Each file contains one electric field spectrogram from each of three instruments: RAD1 (radio receiver band 1), RAD2 (radio receiver band 2) and TNR (thermal noise receiver). The intensity values are color coded and are expressed as tlm counts above galactic background for the RAD1 and RAD2 receivers and as dB below a volt per root Hz for the TNR. Each plot spans 24 hours. Above the RAD2 spectrogram are spacecraft GSE coordinates at the beginning and ending of the time period of the plot. RAD1 PLOT RAD1 is the low frequency radio astronomy receiver. It sweeps over the range of 20 to 1040 kHz with as many as 256 channels. However, some of the time the number of channels is restricted to 16 or 32 so that direction of arrival and polarization information can be obtained. RAD2 PLOT RAD2 is the high frequency radio astronomy receiver. It sweeps over the range of 1.075 to 13.825 MHz with as many as 256 channels. However, some of the time the number of channels is restricted to 16 or 32 so that direction of arrival and polarization information can be obtained. TNR PLOT The thermal noise receiver (TNR) is designed to actively track the solar wind plasma frequency. TNR consists of 5 overlapping bands. Each band covers 2 octaves, with the next band beginning at the mid point of the lower band. The overall frequency range is 4 - 256 kHz. Usually the tnr is operated in a mode where the first, third and fifth bands are sampled, but occassionally the instrument is driven by neural network software which tries to pick the one band containing the plasma frequency. At the bottom are panels showing the AGC level of each band and it can be determined from these just which mode of operation exists. The main plot is in the form of a dynamic spectra with intensity shown as a color bar. The units are db below a volt per root Hz. Information on the instrument and antenna status is also provided below the TNR spectrogram. |

20) | Wind Radio/Plasma Wave, (WAVES) Hi-Res Parameters CDF | |||||||||||||||||
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Resource ID:spase://VWO/NumericalData/Wind/WAVES/DS.PT1M | ||||||||||||||||||

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Wind Waves RAD2, RAD1, and TNR data in CDF format. RAD1 RAD1 is the low frequency radio astronomy receiver. It sweeps over the range of 20 to 1040 kHz with as many as 256 channels. However, some of the time the number of channels is restricted to 16 or 32 so that direction of arrival and polarization information can be obtained. RAD2 RAD2 is the high frequency radio astronomy receiver. It sweeps over the range of 1.075 to 13.825 MHz with as many as 256 channels. However, some of the time the number of channels is restricted to 16 or 32 so that direction of arrival and polarization information can be obtained. TNR The thermal noise receiver (TNR) is designed to actively track the solar wind plasma frequency. TNR consists of 5 overlapping bands. Each band covers 2 octaves, with the next band beginning at the mid point of the lower band. The overall frequency range is 4 - 256 kHz. Usually the tnr is operated in a mode where the first, third and fifth bands are sampled, but occassionally the instrument is driven by neural network software which tries to pick the one band containing the plasma frequency. For more information: The Radio and Plasma Wave Investigation on the Wind Spacecraft, Sp.Sci.Rev.,Vol 71, pg, 231-263,1995 |

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