Showing 1 - 30 |

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) | AMPTE/UKS Ion Plasma Data | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/AMPTE_UKS/Plasma/FTR_PT5S | ||||||||||||||||||

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AMPTE/UKS 5-second (spin) averaged ion plasma moments |

3) | AMPTE/UKS Ion Plasma Data, solar wind mode | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/AMPTE_UKS/Plasma/SWI_PT5S | ||||||||||||||||||

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AMPTE/UKS 5-second (spin) averaged ion plasma moments |

4) | Cluster II Salsa Prime Parameter Plasma Electron and Current Experiment (PEACE) Data | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Cluster-Salsa/PEACE/PrimeParameter/4S | ||||||||||||||||||

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The primary task of this instrument (PEACE: Plasma Electrons and Currents Experiment) is to obtain the velocity moments of the distribution function of electrons as frequently and as accurately as the spacecraft telemetry will allow. Detector counts are collected in energy, polar-angle, and azimuth-angle bins to form a three-dimensional matrix. Two sensors are used: LEEA (low-energy electron analyzer) and HEEA (high-energy electron analyzer). The energy coverage is from 0.67 eV to 30 KeV in 92 levels. The first 16 levels are equally spaced linearly up to 10.7 eV; the remainder are logarithmically spaced. Both sensors can use the full range, but the HEEA will normally operate over a higher energy range than the LEEA. The LEEA specializes in coverage of the energies from 0.7-10 eV, and has a geometric factor one fifth that of the HEAA. Both sensors consist of hemispherical electrostatic analyzers of the top-hat type and a detector in the form of an annular micro-channel plate with a position-sensitive readout. Each sensor covers the range 0-180 degrees with respect to the spin axis, and they are mounted opposite each other with a view perpendicular to the spin axis, thus covering the complete angular range in a half rotation of the spacecraft. The field of view perpendicular to the fan is 2 degrees for the LEEA and 5.6 degrees for the HEEA. Energy resolution (Delta-E)/E is 0.13 for LEEA and 0.16 for HEEA. There are four sweep modes, synchronized to the spin period (4 s), to vary the azimuthal angular resolution. The spin phasing can be made coincident with that of the CIS instrument, to ensure that the electron and ion moments will be measured simultaneously. On-board processing is used to calculate the moments of the distribution with an accuracy of 1% and to select suitable parts of the complete distribution for transmission. The normal science data format is based on one spin period, and consists of core data followed by other optional distributions as can be fit into the available telemetry for that spin. The core data (moments, spacecraft potential, and pitch angle distribution) are always transmitted (if the spin is nominal). The next distribution is transmitted if, before the end of the spin, all the previous data have been sent. Thus the next spin of data will be transmitted slightly late, but all of its core data will be transmitted before the following spin of data is started on. Eventually the transmission will catch up and be able to transmit the distribution after the core again, but only after some time. This applies at all telemetry rates. The instrument can adapt automatically to six different telemetry rates: a basic 1.52 Kbps rate (CIS priority); a normal 2.52 Kbps rate; an enhanced PEACE priority rate of 3.54 Kbps; and three burst mode rates, with a maximum of 15.98 Kbps. For more details of the Cluster mission, the spacecraft, and its instruments, see the report Cluster: mission, payload and supporting activities, March 1993, ESA SP-1159, and the included article PEACE: a Plasma Electron and Current Experiment, by A. D. Johnstone et al., from which this information was obtained. |

5) | Cluster II Salsa Prime Parameter Waves of HF and Sounder for Probing Electron Density by Relaxation (WHISPER) Data | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Cluster-Salsa/WHISPER/PrimeParameter/4S | ||||||||||||||||||

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The Waves of HF and Sounder for Probing Electron Density by Relaxation (WHISPER) experiment provides measurements of the electron density via active sounding of plasma resonances and records via passive wave analysis the natural wave emissions in the high-frequency range, from 4-80 KHz. For more details of the Cluster mission, the spacecraft, and its instruments, see the report Cluster: mission, payload and supporting activities, March 1993, ESA SP-1159, and the included article WHISPER, a Sounder and High-Frequency Wave Analyser Experiment, by P. M. E. Decreau et al., from which this information was obtained. |

6) | Cluster II Summary Parameter Plasma Electron and Current Experiment (PEACE) Data | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Cluster/PEACE/SummaryParameter/60S | ||||||||||||||||||

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The primary task of this instrument (PEACE: Plasma Electrons and Currents Experiment) is to obtain the velocity moments of the distribution function of electrons as frequently and as accurately as the spacecraft telemetry will allow. Detector counts are collected in energy, polar-angle, and azimuth-angle bins to form a three-dimensional matrix. Two sensors are used: LEEA (low-energy electron analyzer) and HEEA (high-energy electron analyzer). The energy coverage is from 0.67 eV to 30 KeV in 92 levels. The first 16 levels are equally spaced linearly up to 10.7 eV; the remainder are logarithmically spaced. Both sensors can use the full range, but the HEEA will normally operate over a higher energy range than the LEEA. The LEEA specializes in coverage of the energies from 0.7-10 eV, and has a geometric factor one fifth that of the HEAA. Both sensors consist of hemispherical electrostatic analyzers of the top-hat type and a detector in the form of an annular micro-channel plate with a position-sensitive readout. Each sensor covers the range 0-180 degrees with respect to the spin axis, and they are mounted opposite each other with a view perpendicular to the spin axis, thus covering the complete angular range in a half rotation of the spacecraft. The field of view perpendicular to the fan is 2 degrees for the LEEA and 5.6 degrees for the HEEA. Energy resolution (Delta-E)/E is 0.13 for LEEA and 0.16 for HEEA. There are four sweep modes, synchronized to the spin period (4 s), to vary the azimuthal angular resolution. The spin phasing can be made coincident with that of the CIS instrument, to ensure that the electron and ion moments will be measured simultaneously. On-board processing is used to calculate the moments of the distribution with an accuracy of 1% and to select suitable parts of the complete distribution for transmission. The normal science data format is based on one spin period, and consists of core data followed by other optional distributions as can be fit into the available telemetry for that spin. The core data (moments, spacecraft potential, and pitch angle distribution) are always transmitted (if the spin is nominal). The next distribution is transmitted if, before the end of the spin, all the previous data have been sent. Thus the next spin of data will be transmitted slightly late, but all of its core data will be transmitted before the following spin of data is started on. Eventually the transmission will catch up and be able to transmit the distribution after the core again, but only after some time. This applies at all telemetry rates. The instrument can adapt automatically to six different telemetry rates: a basic 1.52 Kbps rate (CIS priority); a normal 2.52 Kbps rate; an enhanced PEACE priority rate of 3.54 Kbps; and three burst mode rates, with a maximum of 15.98 Kbps. For more details of the Cluster mission, the spacecraft, and its instruments, see the report Cluster: mission, payload and supporting activities, March 1993, ESA SP-1159, and the included article PEACE: a Plasma Electron and Current Experiment, by A. D. Johnstone et al., from which this information was obtained. |

7) | Cluster II Summary Parameter Waves of HF and Sounder for Probing Electron Density by Relaxation (WHISPER) Data | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Cluster/WHISPER/SummaryParameter/60S | ||||||||||||||||||

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The Waves of HF and Sounder for Probing Electron Density by Relaxation (WHISPER) experiment provides measurements of the electron density via active sounding of plasma resonances and records via passive wave analysis the natural wave emissions in the high-frequency range, from 4-80 KHz. For more details of the Cluster mission, the spacecraft, and its instruments, see the report Cluster: mission, payload and supporting activities, March 1993, ESA SP-1159, and the included article WHISPER, a Sounder and High-Frequency Wave Analyser Experiment, by P. M. E. Decreau et al., from which this information was obtained. |

8) | Dynamics Explorer 2 Ion Drift Meter (IDM) | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/DE2/IDM/PT0.25S | ||||||||||||||||||

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Dynamics Explorer 2 Ion Drift Meter (IDM) |

9) | Dynamics Explorer 2 Langmuir Probe (LANG) | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/DE2/LANG/PT0.5S | ||||||||||||||||||

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Dynamics Explorer 2 Langmuir Probe (LANG) |

10) | Dynamics Explorer 2 Retarding Potential Analyzer (RPA) | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/DE2/VEFI/Ni.Vi.Ti/PT2S | ||||||||||||||||||

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Dynamics Explorer 2 Retarding Potential Analyzer (RPA) |

11) | Dynamics Explorer 2 Retarding Potential Analyzer (RPA) | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/DE2/VEFI/Ni/PT0.016S | ||||||||||||||||||

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Dynamics Explorer 2 Retarding Potential Analyzer (RPA) |

12) | Double Star 1 Spacecraft Hot Ion Analyzer (HIA) Prime Parameters Data | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/DoubleStar1/HIA/PrimeParameters/4S | ||||||||||||||||||

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The Double Star 1 Hot Ion Analyzer (HIA) prime parameter data set contains various parameters at spin resolution. These parameters include universal time, the instrument status, the ion density, ion bulk velocity, and ion temperature. These parameters are available through Double Star Science Data Centre The Data Ring with restricted access. |

13) | Double Star 1 Spacecraft Hot Ion Analyzer (HIA) Summary Parameters Data | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/DoubleStar1/HIA/SummaryParameters/60S | ||||||||||||||||||

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The Double Star 1 Hot Ion Analyzer (HIA) summary parameter data set contains various parameters at 60 s resolution. These parameters include universal time, the instrument status, the ion density, ion bulk velocity, and ion temperature. These parameters are available through Double Star Science Data Centre The Data Ring with restricted access. |

14) | Double Star 1 Spacecraft Data Plasma Electron and Current Experiment (PEACE) Prime Parameters Data | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/DoubleStar1/PEACE/PrimeParameters/4S | ||||||||||||||||||

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The Double Star 1 Plasma Electron and Current Experiment (PEACE) prime parameter data set contains various parameters at spin resolution. These parameters include universal time, the instrument status, the electron density, electron bulk velocity, electron temperature, and electron heat flux. These parameters are available through Double Star Science Data Centre The Data Ring with restricted access. |

15) | Double Star 1 Spacecraft Data Plasma Electron and Current Experiment (PEACE) Summary Parameters Data | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/DoubleStar1/PEACE/SummaryParameters/60S | ||||||||||||||||||

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The Double Star 1 Plasma Electron and Current Experiment (PEACE) summary parameter data set contains various parameters at 60 s resolution. These parameters include universal time, the instrument status, the electron density, electron bulk velocity, electron temperature, and electron heat flux. These parameters are available through Double Star Science Data Centre The Data Ring with restricted access. |

16) | ISEE 2 FPE plasma parameters, 6 Re to bow shock | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/ISEE2/FPE/PT1M | ||||||||||||||||||

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TBD |

17) | PolarEFI_Burst_SC_Potential_PlasmaDensity | |||||||||||||||||
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Resource ID:
spase://VWO/NumericalData/POLAR/EFI/SC_Potential_PlasmaDensity_Burst
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This data consists of the Spacecraft Potential and the Plasma Density, at spacecraft burst resolution, where the Plasma Density is obtained as a function, provided by Dr. Jack Scudder, the PI of the POLAR Hydra investigation. This function was determined by a fit to the POLAR Hydra particle data for 2001/04/01. The relative accuracy of the Plasma Density, estimated from the spacecraft potential on short time scales is ~10-30% depending on plasma conditions. The absolute accuracy is better than a factor of two for densities less than about 20 particles/cm^3. Density values greater than 30 particles/cm^3 are not plotted because they are inaccurate due to the steep slope of the curve of density versus spacecraft potential. If the value of the argument to the function is too large, then the Plasma Density is set to a filler value of 1.0e+20. Also, if the value returned by the function is too large, then the result is not reliable, and therefore the Plasma Density is set to a filler value of 1.0e+20. If the value of the argument to the function is too small, then the Plasma Density is set to a filler value of 1.0e-20. So, a value of the Plasma Density is a filler value if and only if it is either larger than 1.0e+2 (100.0) or smaller than 1.0e-4 (0.0001); otherwise, it is a true value. Note that all values of the Spacecraft Potential are true values. There is no filler. |

18) | PolarEFI_Burst_SC_Potential_PlasmaDensity | |||||||||||||||||
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Resource ID:
spase://SMWG/NumericalData/POLAR/EFI/SC_Potential_PlasmaDensity_Burst
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This data consists of the Spacecraft Potential and the Plasma Density, at spacecraft burst resolution, where the Plasma Density is obtained as a function, provided by Dr. Jack Scudder, the PI of the POLAR Hydra investigation. This function was determined by a fit to the POLAR Hydra particle data for 2001/04/01. The relative accuracy of the Plasma Density, estimated from the spacecraft potential on short time scales is ~10-30% depending on plasma conditions. The absolute accuracy is better than a factor of two for densities less than about 20 particles/cm^3. Density values greater than 30 particles/cm^3 are not plotted because they are inaccurate due to the steep slope of the curve of density versus spacecraft potential. If the value of the argument to the function is too large, then the Plasma Density is set to a filler value of 1.0e+20. Also, if the value returned by the function is too large, then the result is not reliable, and therefore the Plasma Density is set to a filler value of 1.0e+20. If the value of the argument to the function is too small, then the Plasma Density is set to a filler value of 1.0e-20. So, a value of the Plasma Density is a filler value if and only if it is either larger than 1.0e+2 (100.0) or smaller than 1.0e-4 (0.0001); otherwise, it is a true value. Note that all values of the Spacecraft Potential are true values. There is no filler. |

19) | PolarEFI_Realtime_SC_Potential_PlasmaDensity | |||||||||||||||||
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Resource ID:
spase://VWO/NumericalData/POLAR/EFI/SC_Potential_PlasmaDensity_Realtime
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This data consists of the Spacecraft Potential and the Plasma Density, at spacecraft realtime resolution, where the Plasma Density is obtained as a function, provided by Dr. Jack Scudder, the PI of the POLAR Hydra investigation. This function was determined by a fit to the POLAR Hydra particle data for 2001/04/01. The relative accuracy of the Plasma Density, estimated from the spacecraft potential on short time scales is ~10-30% depending on plasma conditions. The absolute accuracy is better than a factor of two for densities less than about 20 particles/cm^3. Density values greater than 30 particles/cm^3 are not plotted because they are inaccurate due to the steep slope of the curve of density versus spacecraft potential. If the value of the argument to the function is too large, then the Plasma Density is set to a filler value of 1.0e+20. Also, if the value returned by the function is too large, then the result is not reliable, and therefore the Plasma Density is set to a filler value of 1.0e+20. If the value of the argument to the function is too small, then the Plasma Density is set to a filler value of 1.0e-20. So, a value of the Plasma Density is a filler value if and only if it is either larger than 1.0e+2 (100.0) or smaller than 1.0e-4 (0.0001); otherwise, it is a true value. Note that all values of the Spacecraft Potential are true values. There is no filler. |

20) | PolarEFI_Realtime_SC_Potential_PlasmaDensity | |||||||||||||||||
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Resource ID:
spase://SMWG/NumericalData/POLAR/EFI/SC_Potential_PlasmaDensity_Realtime
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This data consists of the Spacecraft Potential and the Plasma Density, at spacecraft realtime resolution, where the Plasma Density is obtained as a function, provided by Dr. Jack Scudder, the PI of the POLAR Hydra investigation. This function was determined by a fit to the POLAR Hydra particle data for 2001/04/01. The relative accuracy of the Plasma Density, estimated from the spacecraft potential on short time scales is ~10-30% depending on plasma conditions. The absolute accuracy is better than a factor of two for densities less than about 20 particles/cm^3. Density values greater than 30 particles/cm^3 are not plotted because they are inaccurate due to the steep slope of the curve of density versus spacecraft potential. If the value of the argument to the function is too large, then the Plasma Density is set to a filler value of 1.0e+20. Also, if the value returned by the function is too large, then the result is not reliable, and therefore the Plasma Density is set to a filler value of 1.0e+20. If the value of the argument to the function is too small, then the Plasma Density is set to a filler value of 1.0e-20. So, a value of the Plasma Density is a filler value if and only if it is either larger than 1.0e+2 (100.0) or smaller than 1.0e-4 (0.0001); otherwise, it is a true value. Note that all values of the Spacecraft Potential are true values. There is no filler. |

21) | PolarEFI_SpinResolution_SC_Potential_PlasmaDensity | |||||||||||||||||
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Resource ID:
spase://SMWG/NumericalData/POLAR/EFI/SC_Potential_PlasmaDensity_Spin
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This data consists of the Spacecraft Potential and the Plasma Density, at spacecraft spin resolution, where the Plasma Density is obtained as a function, provided by Dr. Jack Scudder, the PI of the POLAR Hydra investigation. This function was determined by a fit to the POLAR Hydra particle data for 2001/04/01. The relative accuracy of the Plasma Density, estimated from the spacecraft potential on short time scales is ~10-30% depending on plasma conditions. The absolute accuracy is better than a factor of two for densities less than about 20 particles/cm^3. Density values greater than 30 particles/cm^3 are not plotted because they are inaccurate due to the steep slope of the curve of density versus spacecraft potential. If the value of the argument to the function is too large, then the Plasma Density is set to a filler value of 1.0e+20. Also, if the value returned by the function is too large, then the result is not reliable, and therefore the Plasma Density is set to a filler value of 1.0e+20. If the value of the argument to the function is too small, then the Plasma Density is set to a filler value of 1.0e-20. So, a value of the Plasma Density is a filler value if and only if it is either larger than 1.0e+2 (100.0) or smaller than 1.0e-4 (0.0001); otherwise, it is a true value. Note that all values of the Spacecraft Potential are true values. There is no filler. |

22) | PolarEFI_SpinResolution_SC_Potential_PlasmaDensity | |||||||||||||||||
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Resource ID:
spase://VWO/NumericalData/POLAR/EFI/SC_Potential_PlasmaDensity_Spin
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This data consists of the Spacecraft Potential and the Plasma Density, at spacecraft spin resolution, where the Plasma Density is obtained as a function, provided by Dr. Jack Scudder, the PI of the POLAR Hydra investigation. This function was determined by a fit to the POLAR Hydra particle data for 2001/04/01. The relative accuracy of the Plasma Density, estimated from the spacecraft potential on short time scales is ~10-30% depending on plasma conditions. The absolute accuracy is better than a factor of two for densities less than about 20 particles/cm^3. Density values greater than 30 particles/cm^3 are not plotted because they are inaccurate due to the steep slope of the curve of density versus spacecraft potential. If the value of the argument to the function is too large, then the Plasma Density is set to a filler value of 1.0e+20. Also, if the value returned by the function is too large, then the result is not reliable, and therefore the Plasma Density is set to a filler value of 1.0e+20. If the value of the argument to the function is too small, then the Plasma Density is set to a filler value of 1.0e-20. So, a value of the Plasma Density is a filler value if and only if it is either larger than 1.0e+2 (100.0) or smaller than 1.0e-4 (0.0001); otherwise, it is a true value. Note that all values of the Spacecraft Potential are true values. There is no filler. |

23) | SCATHA Science Summary Data | |||||||||||||||||
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Resource ID:spase://ViRBO/NumericalData/SCATHA/SC1/SC2/SC3/SC4/SC10/SC11/PT1M | ||||||||||||||||||

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SCATHA Science Summary Data |

24) | SCATHA Science Full Resolution Data | |||||||||||||||||
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Resource ID:spase://ViRBO/NumericalData/SCATHA/SC1/SC2/SC3/SC4/SC10/SC11/PT1S | ||||||||||||||||||

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SCATHA Science Full Resolution Data |

25) | SOHO CELIAS 5-min Key Parameter Data | |||||||||||||||||
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Resource ID:spase://VEPO/NumericalData/SOHO/CELIAS/KP/PT5M | ||||||||||||||||||

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Data include 5-min solar wind speed values, heavy ion fluxes in energy bands 0.02-1. MeV/q and 0.5-50 keV/q, and solar EUV photon fluxes from the CELIAS package on SOHO. They are key parameter data accessible from CDAWeb. Scanning CDAWeb plots for the full 1995-2002 time span suggests that only the solar wind flow speed are useful |

26) | VOYAGER 1 SOLAR WIND PLS 1 HOUR AVERAGES V1.0 | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Voyager1/PLS/Heliosphere/PT1H | ||||||||||||||||||

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Voyager 1 plasma data of the solar wind, 1 hour averages. The files in this directory contain the Voyager hourly average plasma data. The plasma parameters are obtained by finding the best fit of a convected isotropic Maxwellian distribution to the data. One sigma errors are typically less than 0.5% in the speed and VR, less than 5% for the density and thermal speed, and vary greatly for VT and VN. Sampling times range from 12 to 192 sec., with sampling generally more frequent early in the mission. The columns are: 1) Year 2) day of year (day 1 is Jan. 1) 3) hour 4) proton speed in km/s (magnitude of V) 5) proton density in cm-3 6) proton thermal speed in km/s (proton temperature in eV = .0052 times the square of the thermal speed) 7) VR 8) VT (WARNING: this parameter is often NOT reliable after 1989) 9) VN (WARNING: this parameter is often NOT reliable after 1989) The velocity components are given in the RTN coordinate system, where R is radially outward, T is in a plane parallel to the solar equatorial plane and positive in the direction of solar rotation, and N completes a right-handed system. Please consult with us, or at least send preprints, when you use this data to prevent grievous errors or misconceptions. (John Richardson, jdr@space.mit.edu) |

27) | VOYAGER 1 SOLAR WIND PLS FINE RES V1.0 | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Voyager1/PLS/Heliosphere/PT96S | ||||||||||||||||||

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Voyager 1 plasma data of the solar wind, fine resolution data. The files in this directory contain the Voyager fine resolution plasma data. The plasma parameters are obtained by finding the best fit of a convected isotropic Maxwellian distribution to the data. One sigma errors are typically less than 0.5 percent in the speed and VR, less than 5 percent for the density and thermal speed, and vary greatly for VT and VN. Sampling times range from 12 to 192 sec., with sampling generally more frequent early in the mission. The columns are: 1) Year 2) day of year (day 1 is Jan. 1) 3) decimal hour 4) proton speed in km/s (magnitude of V) 5) proton density in cm-3 6) proton thermal speed in km/s (proton temperature in eV = .0052 times the square of the thermal speed) 7) VR 8) VT (WARNING: this parameter is often NOT reliable after 1989) 9) VN (WARNING: this parameter is often NOT reliable after 1989) The velocity components are given in the RTN coordinate system, where R is radially outward, T is in a plane parallel to the solar equatorial plane and positive in the direction of solar rotation, and N completes a right-handed system. Please consult with us, or at least send preprints, when you use this data to prevent grievous errors or misconceptions. (John Richardson, jdr@space.mit.edu) |

28) | VG1 JUP PLS PLASMA DERIVED ION MOMENTS 96.0 SEC V1.1 | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Voyager1/PLS/Jupiter/PT96.0S | ||||||||||||||||||

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Data Set Overview ================= Version 1.1 ----------- This version 1.1 data set replaces the version 1.0 data set (DATA_SET_ID = VG1-J-PLS-5-ION-MOM-96.0SEC) previously archived with the PDS. Data Set Description -------------------- This data set contains the best estimates of the total ion density at Jupiter during the Voyager 1 encounter in the PLS voltage range (10-5950 eV/Q). It is calculated using the method of [MCNUTTETAL1981] which to first order consists of taking the total measured current and dividing by the collector area and plasma bulk velocity. This method is only accurate for high mach number flows directly into the detector, and may result in underestimates of the total density of a factor of 2 in the outer magnetosphere. Thus absolute densities should be treated with caution, but density variations in the data set can be trusted. The low resolution mode density is used before 1979 63 1300, after this the larger of the high and low resolution mode densities in a 96 sec period is used since the L-mode spectra often are saturated. Corotation is assumed inside L=17.5, and a constant velocity component of 200 km/s into the D cup is used outside of this. These are the densities given in [MCNUTTETAL1981] corrected by a factor of 1.209 (.9617) for densities obtained from the side (main) sensor. This correction is due to a better calculation of the effective area of the sensors. Data format: column 1 is time (yyyy-mm-ddThh:mm:ss.sssZ), column 2 is the moment density in cm^-3. Each row has format (a24, 1x, 1pe9.2). Values of -9.99e+10 indicate that the parameter could not be obtained from the data using the standard analysis technique. Additional information about this data set and the instrument which produced it can be found elsewhere in this catalog. An overview of the data in this data set can be found in [MCNUTTETAL1981] and a complete instrument description can be found in [BRIDGEETAL1977]. Processing Level Id : 5 Software Flag : Y Parameters ========== Ion Density ----------- Sampling Parameter Name : TIME Data Set Parameter Name : ION DENSITY Sampling Parameter Resolution : 96.000000 Sampling Parameter Interval : 96.000000 Minimum Available Sampling Int : 96.000000 Data Set Parameter Unit : EV Sampling Parameter Unit : SECOND A derived parameter equaling the number of ions per unit volume over a specified range of ion energy, energy/charge, or energy/nucleon. Discrimination with regard to mass and or charge state is necessary to obtain this quantity, however, mass and charge state are often assumed due to instrument limitations. Many different forms of ion density are derived. Some are distinguished by their composition (N+, proton, ion, etc.) or their method of derivation (Maxwellian fit, method of moments). In some cases, more than one type of density will be provided in a single data set. In general, if more than one ion species is analyzed, either by moment or fit, a total density will be provided which is the sum of the ion densities. If a plasma component does not have a Maxwellian distribution the actual distribution can be represented as the sum of several Maxwellians, in which case the density of each Maxwellian is given. Source Instrument Parameters ============================ Instrument Host ID : VG1 Data Set Parameter Name : ION DENSITY Instrument Parameter Name : ION RATE ION CURRENT PARTICLE MULTIPLE PARAMETERS Important Instrument Parameters : 1 (for all parameters) Processing ========== Processing History ------------------ Source Data Set ID : VG1-PLS Software : MOMANAL Product Data Set ID : VG1-J-PLS-5-ION-MOM-96.0SEC Software 'MOMANAL' ------------------ Software |

29) | VG1 JUP PLS DERIVED ION OUTBND MAGSHTH M-MODE 96SEC V1.0 | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Voyager1/PLS/Jupiter/PT96S | ||||||||||||||||||

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Data Set Overview ================= Instrument P.I. : John D. Richardson Data Supplier : John D. Richardson Data sampling rate : 96 seconds Data Set Start Time : 1979-03-13T00:01:43.491Z Data Set Stop Time : 1979-03-24T23:20:06.519Z This data set contains plasma parameters from Voyager 1 outbound from Jupiter from the magnetotail through the solar wind. Fit and moment parameters are given; the fit parameters assume a single, isotropic convected proton Maxwellian distribution. Although magnetotail data is provided, these data are unreliable; the density can be used as an upper limit to the actual density. Solar wind data are also provided and are reliable. These M mode data are the best data to use in most regions of the magnetosheath. Magnetotail data in this data set are included mainly to put the sheath data in context and show magnetopause. Parameters ========== Data Set Parameter 'ION DENSITY' -------------------------------- Data Set Parameter Name : ION DENSITY Data Set Parameter Unit : CM**-3 Sampling Parameter Name : TIME Sampling Parameter Unit : SECOND Minimum Sampling Parameter : UNK Maximum Sampling Parameter : UNK Sampling Parameter Interval : UNK Minimum Available Sampling Int : UNK Noise Level : UNK A derived parameter equaling the number of ions per unit volume over a specified range of ion energy, energy/charge, or energy/nucleon. Discrimination with regard to mass and or charge state is necessary to obtain this quantity, however, mass and charge state are often assumed due to instrument limitations. Many different forms of ion density are derived. Some are distinguished by their composition (N+, proton, ion, etc.) or their method of derivation (Maxwellian fit, method of moments). In some cases, more than one type of density will be provided in a single data set. In general, if more than one ion species is analyzed, either by moment or fit, a total density will be provided which is the sum of the ion densities. If a plasma component does not have a Maxwellian distribution the actual distribution can be represented as the sum of several Maxwellians, in which case the density of each Maxwellian is given. Data Set Parameter 'ION THERMAL SPEED' -------------------------------------- Data Set Parameter Name : ION THERMAL SPEED Data Set Parameter Unit : KM/S Sampling Parameter Name : TIME Sampling Parameter Unit : SECOND Minimum Sampling Parameter : UNK Maximum Sampling Parameter : UNK Sampling Parameter Interval : UNK Minimum Available Sampling Int : UNK Noise Level : UNK A measure of the velocity associated with the temperature of the ions. It is formally defined as the Ion Thermal Speed squared equals two times K (Boltzmann's constant) times T (temperature of ion) divided by M (ion mass). Each component of a plasma has a thermal speed associated with it. Data Set Parameter 'ION VELOCITY' --------------------------------- Data Set Parameter Name : ION VELOCITY Data Set Parameter Unit : KM/S Sampling Parameter Name : TIME Sampling Parameter Unit : SECOND Minimum Sampling Parameter : UNK Maximum Sampling Parameter : UNK Sampling Parameter Interval : UNK Minimum Available Sampling Int : UNK Noise Level : UNK A derived parameter giving the average speed and direction of motion of a plasma or plasma component. The velocity can be obtained by taking the first moment of the distribution function or by simulating the observations with some known distribution function, usually a Maxwellian, to the distribution. Velocities are given in heliographic (RTN) coordinates: R is radially away from sun, T is in plane of sun's equator and positive in the direction of solar rotation, N completes right-handed system. Source Instrument Parameters ============================ Instrument Host ID : VG1 Data Set Parameter Name : ION DENSITY Instrument Parameter Name : ION RATE Important Instrument Parameters : 1 Instrument Host ID : VG1 Data Set Parameter Name : ION DENSITY Instrument Parameter Name : ION CURRENT Important Instrument Parameters : 1 Instrument Host ID : VG1 Data Set Parameter Name : ION VELOCITY Instrument Parameter Name : ION CURRENT Important Instrument Parameters : 1 Instrument Host ID : VG1 Data Set Parameter Name : ION THERMAL SPEED Instrument Parameter Name : ION RATE Important Instrument Parameters : 1 Instrument Host ID : VG1 Data Set Parameter Name : ION THERMAL SPEED Instrument Parameter Name : ION CURRENT Important Instrument Parameters : 1 Instrument Host ID : VG1 Data Set Parameter Name : ION DENSITY Instrument Parameter Name : PARTICLE MULTIPLE PARAMETERS Important Instrument Parameters : 1 Data Coverage ============= Filename Records Start Stop ------------------------------------------------------------------- T79072 10232 1979-03-13T00:01:43.491Z 1979-03-24T23:20:06.519Z |

30) | VG1 SAT PLS DERIVED ION SOLAR WIND BROWSE 96SEC V1.0 | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Voyager1/PLS/Saturn/PT96S | ||||||||||||||||||

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Data Set Overview ================= Instrument P.I. : John D. Richardson Data Supplier : John D. Richardson Data sampling rate : 96 seconds Data Set Start Time : 1981-08-19T00:00:09.229Z Data Set Stop Time : 1981-09-04T02:51:21.885Z This data set contains solar wind plasma browse data near the Voyager 1 Saturn encounter. Moment parameters are given. Since only the first 72 or last 72 energy/charge channels are telemetered to Earth from each M-mode spectra, derived parameters change significantly only every other set of spectra so the effective time resolution is 96 second. Parameters ========== Data Set Parameter 'ION DENSITY' -------------------------------- Data Set Parameter Name : ION DENSITY Data Set Parameter Unit : CM**-3 Sampling Parameter Name : TIME Sampling Parameter Unit : SECOND Minimum Sampling Parameter : UNK Maximum Sampling Parameter : UNK Sampling Parameter Interval : UNK Minimum Available Sampling Int : UNK Noise Level : UNK A derived parameter equaling the number of ions per unit volume over a specified range of ion energy, energy/charge, or energy/nucleon. Discrimination with regard to mass and or charge state is necessary to obtain this quantity, however, mass and charge state are often assumed due to instrument limitations. Many different forms of ion density are derived. Some are distinguished by their composition (N+, proton, ion, etc.) or their method of derivation (Maxwellian fit, method of moments). In some cases, more than one type of density will be provided in a single data set. In general, if more than one ion species is analyzed, either by moment or fit, a total density will be provided which is the sum of the ion densities. If a plasma component does not have a Maxwellian distribution the actual distribution can be represented as the sum of several Maxwellians, in which case the density of each Maxwellian is given. Data Set Parameter 'ION TEMPERATURE' ------------------------------------ Data Set Parameter Name : ION TEMPERATURE Data Set Parameter Unit : EV Sampling Parameter Name : TIME Sampling Parameter Unit : SECOND Minimum Sampling Parameter : UNK Maximum Sampling Parameter : UNK Sampling Parameter Interval : UNK Minimum Available Sampling Int : UNK Noise Level : UNK A derived parameter giving an indication of the mean energy/ion, assuming the shape of the ion energy spectrum to be Maxwellian. Given that the ion energy spectrum is not exactly Maxwellian, the ion temperature can be defined integrally (whereby the mean energy obtained by integrating under the actual ion energy spectrum is set equal to the integral under a Maxwellian, where the temperature is a free parameter for which to solve), or differentially (whereby the slopes of the actually ion energy spectrum at various energies are matched to the slopes of a corresponding Maxwellian). The temperature parameter is often qualified with a range of applicable energies. Temperatures can be angularly anisotropic. If the ions do not have a Maxwellian distribution the actual distribution can be represented as the sum of several Maxwellians, each with a separate temperature. Data Set Parameter 'ION THERMAL SPEED' -------------------------------------- Data Set Parameter Name : ION THERMAL SPEED Data Set Parameter Unit : KM/S Sampling Parameter Name : TIME Sampling Parameter Unit : SECOND Minimum Sampling Parameter : UNK Maximum Sampling Parameter : UNK Sampling Parameter Interval : UNK Minimum Available Sampling Int : UNK Noise Level : UNK A measure of the velocity associated with the temperature of the ions. It is formally defined as the Ion Thermal Speed squared equals two times K (Boltzmann's constant) times T (temperature of ion) divided by M (ion mass). Each component of a plasma has a thermal speed associated with it. Data Set Parameter 'ION VELOCITY' --------------------------------- Data Set Parameter Name : ION VELOCITY Data Set Parameter Unit : KM/S Sampling Parameter Name : TIME Sampling Parameter Unit : SECOND |

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