Showing 1 - 33 |

1) | Akebono TED thermal electron spectral plots | |||||||||||||||||
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Resource ID:spase://VSPO/DisplayData/Akebono/TED/PT8S | ||||||||||||||||||

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These Akebono Thermal Electron Energy Detecftor (TED) plots display color-coded amplitudes of the second harmonic of incident flux, vs. energy (over 0-5 eV) and time. Each plot covers some or all of one ~3.5 hour orbit. |

2) | Akebono TED thermal electron digital spectra | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/Akebono/TED/PT8S | ||||||||||||||||||

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These Akebono Thermal Electron Energy Detecftor (TED) digital data reside at the DARTS/Akebono binary Science Database (SDB). They consist of amplitudes of the second harmonic of incident flux. Data-read software and an algorithms for converting the data to an energy distribution function in units of 1/(eV cm**3) are given in the Information URL cited below. |

3) | Cluster Rumba Digital Wave Processor (DWP) Data at the ESA Cluster Science Archive | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/Cluster-Rumba/DWP/CSA/PT4S | ||||||||||||||||||

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As the central control and data processing unit for the Wave Experiement Consortium (WEC), the Digital Wave Processor (DWP) provided the following products in the Cluster Active Archive: (1) Time correction data (C1_CP_DWP_TCOR) with timing accuracy improved to 20 micro seconds; (2) Summary of the status of the Wave Experiment Consortium (C1_CP_DWP_ LOG) with one record for each interval that the WEC operates in the same mode for a total of 64 parameters including: instrument modes, telemetry use statistics, errors and anomalies, summary of voltage and temperature housekeeping; (3) A listing of the command sequences uplinked to the Wave Experiment Consortium (CM_CD_DWP_UT_PIOR); (4) High resolution particle correlator data for the fixed (pre-selected) energy band (C1_CP_DWP_COR_FX) and high resolution particle correlator data for the stepped energy (C1_CP_ DWP_COR_ST) which steps through the remaining 14 bands, at one step per spin; and (5) Documentation and software. Electron energy range is from 0.6 eV to 26 keV in 15 energy bands (PEACE mode dependent) and frequency range, 1.4 kHz to 41.6 kHz in 32 frequency bands and DC to 4 Hz based on successive autocorrelation function (ACF) outputs. For more details, see "The Cluster Active Archive: Studying the Earth's Space Plasma Environment", edited by Dr. Harri Laakso, Matthew G. T. T. Taylor, C. Philippe Escoubet. |

4) | Cluster Rumba Digital Wave Processor (DWP) prime parameter data at about 4 sec resolution (spin averaged) in GSE Coordinates | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Cluster-Rumba/DWP/PrimeParameter/PT4S | ||||||||||||||||||

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Cluster Rumba Digital Wave Processor (DWP) data set contains various instrument status and data status flags as well as particle correlator information. |

5) | Cluster Salsa Digital Wave Processor (DWP) Data at the ESA Cluster Science Archive | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/Cluster-Salsa/DWP/CSA/PT4S | ||||||||||||||||||

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As the central control and data processing unit for the Wave Experiement Consortium (WEC), the Digital Wave Processor (DWP) provided the following products in the Cluster Active Archive: (1) Time correction data (C1_CP_DWP_TCOR) with timing accuracy improved to 20 micro seconds; (2) Summary of the status of the Wave Experiment Consortium (C1_CP_DWP_ LOG) with one record for each interval that the WEC operates in the same mode for a total of 64 parameters including: instrument modes, telemetry use statistics, errors and anomalies, summary of voltage and temperature housekeeping; (3) A listing of the command sequences uplinked to the Wave Experiment Consortium (CM_CD_DWP_UT_PIOR); (4) High resolution particle correlator data for the fixed (pre-selected) energy band (C1_CP_DWP_COR_FX) and high resolution particle correlator data for the stepped energy (C1_CP_ DWP_COR_ST) which steps through the remaining 14 bands, at one step per spin; and (5) Documentation and software. Electron energy range is from 0.6 eV to 26 keV in 15 energy bands (PEACE mode dependent) and frequency range, 1.4 kHz to 41.6 kHz in 32 frequency bands and DC to 4 Hz based on successive ACF outputs. For more details, see "The Cluster Active Archive: Studying the Earth's Space Plasma Environment", edited by Dr. Harri Laakso, Matthew G. T. T. Taylor, C. Philippe Escoubet. |

6) | Cluster Salsa Digital Wave Processor (DWP) prime parameter data at about 4 sec resolution (spin averaged) in GSE Coordinates | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Cluster-Salsa/DWP/PrimeParameter/PT4S | ||||||||||||||||||

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Cluster Salsa Digital Wave Processor (DWP) data set contains various instrument status and data status flags as well as particle correlator information. |

7) | Cluster Samba Digital Wave Processor (DWP) Data at the ESA Cluster Science Archive | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/Cluster-Samba/DWP/CSA/PT4S | ||||||||||||||||||

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As the central control and data processing unit for the Wave Experiement Consortium (WEC), the Digital Wave Processor (DWP) provided the following products in the Cluster Active Archive: (1) Time correction data (C1_CP_DWP_TCOR) with timing accuracy improved to 20 micro seconds; (2) Summary of the status of the Wave Experiment Consortium (C1_CP_DWP_ LOG) with one record for each interval that the WEC operates in the same mode for a total of 64 parameters including: instrument modes, telemetry use statistics, errors and anomalies, summary of voltage and temperature housekeeping; (3) A listing of the command sequences uplinked to the Wave Experiment Consortium (CM_CD_DWP_UT_PIOR); (4) High resolution particle correlator data for the fixed (pre-selected) energy band (C1_CP_DWP_COR_FX) and high resolution particle correlator data for the stepped energy (C1_CP_ DWP_COR_ST) which steps through the remaining 14 bands, at one step per spin; and (5) Documentation and software. Electron energy range is from 0.6 eV to 26 keV in 15 energy bands (PEACE mode dependent) and frequency range, 1.4 kHz to 41.6 kHz in 32 frequency bands and DC to 4 Hz based on successive autocorrelation function (ACF) outputs. For more details, see "The Cluster Active Archive: Studying the Earth's Space Plasma Environment", edited by Dr. Harri Laakso, Matthew G. T. T. Taylor, C. Philippe Escoubet. |

8) | Cluster Samba Digital Wave Processor (DWP) prime parameter data at about 4 sec resolution (spin averaged) in GSE Coordinates | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Cluster-Samba/DWP/PrimeParameter/PT4S | ||||||||||||||||||

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Cluster Samba Digital Wave Processor (DWP) data set contains various instrument status and data status flags as well as particle correlator information. |

9) | Cluster Tango Digital Wave Processor (DWP) Data at the ESA Cluster Science Archive | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/Cluster-Tango/DWP/CSA/PT4S | ||||||||||||||||||

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As the central control and data processing unit for the Wave Experiement Consortium (WEC), the Digital Wave Processor (DWP) provided the following products in the Cluster Active Archive: (1) Time correction data (C1_CP_DWP_TCOR) with timing accuracy improved to 20 micro seconds; (2) Summary of the status of the Wave Experiment Consortium (C1_CP_DWP_ LOG) with one record for each interval that the WEC operates in the same mode for a total of 64 parameters including: instrument modes, telemetry use statistics, errors and anomalies, summary of voltage and temperature housekeeping; (3) A listing of the command sequences uplinked to the Wave Experiment Consortium (CM_CD_DWP_UT_PIOR); (4) High resolution particle correlator data for the fixed (pre-selected) energy band (C1_CP_DWP_COR_FX) and high resolution particle correlator data for the stepped energy (C1_CP_ DWP_COR_ST) which steps through the remaining 14 bands, at one step per spin; and (5) Documentation and software. Electron energy range is from 0.6 eV to 26 keV in 15 energy bands (PEACE mode dependent) and frequency range, 1.4 kHz to 41.6 kHz in 32 frequency bands and DC to 4 Hz based on successive autocorrelation function (ACF) outputs. For more details, see "The Cluster Active Archive: Studying the Earth's Space Plasma Environment", edited by Dr. Harri Laakso, Matthew G. T. T. Taylor, C. Philippe Escoubet. |

10) | Cluster Tango Digital Wave Processor (DWP) prime parameter data at about 4 sec resolution (spin averaged) in GSE Coordinates | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Cluster-Tango/DWP/PrimeParameter/PT4S | ||||||||||||||||||

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Cluster Tango Digital Wave Processor (DWP) data set contains various instrument status and data status flags as well as particle correlator information. |

11) | Cluster Digital Wave Processor (DWP) summary parameter data at about 60 sec resolution (spin averaged) in GSE Coordinates | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/Cluster/DWP/SummaryParameter/PT60S | ||||||||||||||||||

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Cluster Digital Wave Processor (DWP) data set contains various instrument status and data status flags as well as particle correlator information. |

12) | Equator-S Potential Control Device (PDC) 1-min Prime Parameters | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/Equator-S/PCD/PP/PT60S | ||||||||||||||||||

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This data set from Equator-S Potential Control Device (PCD) contains one-minute summary parameters that are given versus time: the ion current; the half-interval between time tags, averaged over the file; and a status flag. |

13) | GOES 10 EPS, 5-min KP Electron, Proton Fluxes | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/GOES/10/SEM/PT300S | ||||||||||||||||||

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GOES 10 Energetic Particle Sensor, Key Parameters, 5-min fluxes of electrons >0.6, >2, >4 MeV and of 0.7-4 MeV protons |

14) | GOES 11 EPS, 5-min KP Electron, Proton Fluxes | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/GOES/11/SEM/PT300S | ||||||||||||||||||

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This data set from GOES 11 Energetic Particle Sensor contains Key Parameters as 5-min fluxes of electrons >0.6, >2, >4 MeV and of 0.7-4 MeV protons. |

15) | GOES 9 EPS, 5-min KP Electron, Proton Fluxes | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/GOES/9/SEM/PT300S | ||||||||||||||||||

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GOES 9 Energetic Particle Sensor, Key Parameters, 5-min fluxes of electrons >0.6, >2, >4 MeV and of 0.7-4 MeV protons |

16) | GOES X-ray Flux Plots | |||||||||||||||||
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Resource ID:spase://VSPO/DisplayData/GOES/SXM/PLOTS | ||||||||||||||||||

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GOES X-ray plots from NOAA/SEC, 3-day plots of 5-min data |

17) | Hinotori Electron Density and Temperature Data | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/Hinotori/PP/PT10.00S | ||||||||||||||||||

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Hinotori electron density and temperature Data at 10-sec resolution |

18) | MMS 1 Digital Signal Processor (DSP) Search Coil Magnetometer (SCM), Magnetic Field Power Spectral Density, Fast Survey | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/MMS/1/FIELDS/DSP/Fast/Level2/MagneticFieldPowerSpectralDensity/PT2S | ||||||||||||||||||

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The MMS magnetic field power spectral density (BPSD) is computed onboard by the Digital Signal Processor (DSP). The fast Fourier transform (FFT) calculation is performed on a digitized version of analog signals from the Search Coil Magnetometer (SCM) in the SCM123 coordinate system (scm1 = - x sensor; scm2 = -z sensor; scm3 = -y sensor). This data product is computed in space from individual components that are not synchronized to the 1 second pulse. Therefore, the timing between channels can be inaccurate by a fraction of a second. The samples times are interval start times taken from the x component. The spectra are calculated via a 1024-point FFT algorithm on piecewise continuous sets of waveform data. Nine signals can be processed simultaneously. Six of the twelve DC-coupled E, DC-coupled V, or SCM signals (16384 samples/s) are selected for spectral processing at 100% duty cycle. In addition, the three AC-coupled signals (262,144 kS/s) each can be processed at 6.25% duty cycle. Each of the nine signals has 16, 1024-point FFT operations every second; the field-programmable gate array (FPGA) performs 144 FFTs per second. The FFT is performed by an arithmetic logic unit (ALU), which is controlled by a state machine. Both are hard-coded into the FPGA. The operation starts by applying a 1024-point Hanning window onto a waveform. Next, an FFT is implemented. The FFT is broken into a series of "butterfly" operations performed by the ALU. The result has real and imaginary data. Power spectra are calculated by taking the sum of squares of real and imaginary values (the ALU includes a multiplier), which produces a power spectrum with 512 frequency bins. The frequency bins are then combined to give pseudo-logarithmic frequency spacing (del f)/f. The spectra are reduced to 88 frequency bins with (del f)/f between 6% and 12% when possible. Narrow-band emissions can be fit to an accuracy of (del f)/f ~3%, allowing for an accurate determination of plasma density. The spectra can be averaged in time. The fastest reporting rate of any signal is 16 spectra per second. Reporting rates can be as slow a one spectra every 16 s (averaging 256 spectra). The averaging process has 48-bit accuracy to maximize the dynamic range. The amplitudes undergo a pseudo-logarithmic compression to an 8-bit number representing over 120 dB of dynamic range at ~5% precision. |

19) | MMS 1 Digital Signal Processor (DSP) Search Coil Magnetometer (SCM), Magnetic Field Power Spectral Density, Slow Survey | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/MMS/1/FIELDS/DSP/Slow/Level2/MagneticFieldPowerSpectralDensity/PT16S | ||||||||||||||||||

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The MMS magnetic field power spectral density (BPSD) is computed onboard by the Digital Signal Processor (DSP). The fast Fourier transform (FFT) calculation is performed on a digitized version of analog signals from the Search Coil Magnetometer (SCM) in the SCM123 coordinate system (scm1 = - x sensor; scm2 = -z sensor; scm3 = -y sensor). This data product is computed in space from individual components that are not synchronized to the 1 second pulse. Therefore, the timing between channels can be inaccurate by a fraction of a second. The samples times are interval start times taken from the x component. The spectra are calculated via a 1024-point FFT algorithm on piecewise continuous sets of waveform data. Nine signals can be processed simultaneously. Six of the twelve DC-coupled E, DC-coupled V, or SCM signals (16384 samples/s) are selected for spectral processing at 100% duty cycle. In addition, the three AC-coupled signals (262,144 kS/s) each can be processed at 6.25% duty cycle. Each of the nine signals has 16, 1024-point FFT operations every second; the field-programmable gate array (FPGA) performs 144 FFTs per second. The FFT is performed by an arithmetic logic unit (ALU), which is controlled by a state machine. Both are hard-coded into the FPGA. The operation starts by applying a 1024-point Hanning window onto a waveform. Next, an FFT is implemented. The FFT is broken into a series of "butterfly" operations performed by the ALU. The result has real and imaginary data. Power spectra are calculated by taking the sum of squares of real and imaginary values (the ALU includes a multiplier), which produces a power spectrum with 512 frequency bins. The frequency bins are then combined to give pseudo-logarithmic frequency spacing (del f)/f. The spectra are reduced to 88 frequency bins with (del f)/f between 6% and 12% when possible. Narrow-band emissions can be fit to an accuracy of (del f)/f ~3%, allowing for an accurate determination of plasma density. The spectra can be averaged in time. The fastest reporting rate of any signal is 16 spectra per second. Reporting rates can be as slow a one spectra every 16 s (averaging 256 spectra). The averaging process has 48-bit accuracy to maximize the dynamic range. The amplitudes undergo a pseudo-logarithmic compression to an 8-bit number representing over 120 dB of dynamic range at ~5% precision. |

20) | MMS 2 Digital Signal Processor (DSP) Search Coil Magnetometer (SCM), Magnetic Field Power Spectral Density, Fast Survey | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/MMS/2/FIELDS/DSP/Fast/Level2/MagneticFieldPowerSpectralDensity/PT2S | ||||||||||||||||||

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The MMS magnetic field power spectral density (BPSD) is computed onboard by the Digital Signal Processor (DSP). The fast Fourier transform (FFT) calculation is performed on a digitized version of analog signals from the Search Coil Magnetometer (SCM) in the SCM123 coordinate system (scm1 = - x sensor; scm2 = -z sensor; scm3 = -y sensor). This data product is computed in space from individual components that are not synchronized to the 1 second pulse. Therefore, the timing between channels can be inaccurate by a fraction of a second. The samples times are interval start times taken from the x component. The spectra are calculated via a 1024-point FFT algorithm on piecewise continuous sets of waveform data. Nine signals can be processed simultaneously. Six of the twelve DC-coupled E, DC-coupled V, or SCM signals (16384 samples/s) are selected for spectral processing at 100% duty cycle. In addition, the three AC-coupled signals (262,144 kS/s) each can be processed at 6.25% duty cycle. Each of the nine signals has 16, 1024-point FFT operations every second; the field-programmable gate array (FPGA) performs 144 FFTs per second. The FFT is performed by an arithmetic logic unit (ALU), which is controlled by a state machine. Both are hard-coded into the FPGA. The operation starts by applying a 1024-point Hanning window onto a waveform. Next, an FFT is implemented. The FFT is broken into a series of "butterfly" operations performed by the ALU. The result has real and imaginary data. Power spectra are calculated by taking the sum of squares of real and imaginary values (the ALU includes a multiplier), which produces a power spectrum with 512 frequency bins. The frequency bins are then combined to give pseudo-logarithmic frequency spacing (del f)/f. The spectra are reduced to 88 frequency bins with (del f)/f between 6% and 12% when possible. Narrow-band emissions can be fit to an accuracy of (del f)/f ~3%, allowing for an accurate determination of plasma density. The spectra can be averaged in time. The fastest reporting rate of any signal is 16 spectra per second. Reporting rates can be as slow a one spectra every 16 s (averaging 256 spectra). The averaging process has 48-bit accuracy to maximize the dynamic range. The amplitudes undergo a pseudo-logarithmic compression to an 8-bit number representing over 120 dB of dynamic range at ~5% precision. |

21) | MMS 2 Digital Signal Processor (DSP) Search Coil Magnetometer (SCM), Magnetic Field Power Spectral Density, Slow Survey | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/MMS/2/FIELDS/DSP/Slow/Level2/MagneticFieldPowerSpectralDensity/PT16S | ||||||||||||||||||

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22) | MMS 3 Digital Signal Processor (DSP) Search Coil Magnetometer (SCM), Magnetic Field Power Spectral Density, Fast Survey | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/MMS/3/FIELDS/DSP/Fast/Level2/MagneticFieldPowerSpectralDensity/PT2S | ||||||||||||||||||

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23) | MMS 3 Digital Signal Processor (DSP) Search Coil Magnetometer (SCM), Magnetic Field Power Spectral Density, Slow Survey | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/MMS/3/FIELDS/DSP/Slow/Level2/MagneticFieldPowerSpectralDensity/PT16S | ||||||||||||||||||

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24) | MMS 4 Digital Signal Processor (DSP) Search Coil Magnetometer (SCM), Magnetic Field Power Spectral Density, Fast Survey | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/MMS/4/FIELDS/DSP/Fast/Level2/MagneticFieldPowerSpectralDensity/PT2S | ||||||||||||||||||

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25) | MMS 4 Digital Signal Processor (DSP) Search Coil Magnetometer (SCM), Magnetic Field Power Spectral Density, Slow Survey | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/MMS/4/FIELDS/DSP/Slow/Level2/MagneticFieldPowerSpectralDensity/PT16S | ||||||||||||||||||

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26) | SORCE TIM 6-hr and 1-day Total Solar Irradiance | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/SORCE/TIM/PT6H | ||||||||||||||||||

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SORCE TIM 6-hour and daily Total Solar Irradiance Data |

27) | STEREO WAVES (SWAVES) PDF Dynamic Spectrogram Plots both Ahead and Behind s/c | |||||||||||||||||
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Resource ID:spase://VWO/DisplayData/STEREO/SWAVES/DS.Color.PDF.P1D | ||||||||||||||||||

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This dataset contains 24 hour duration dynamic spectrogram plots from the combined STEREO A and B Waves instrument. The plots are provided in several file formats (PNG, Postscript and PDF) and there are renditions in color and grayscale with and without additional lines of time series data indicating the instrument operating status. These plots all reside within the same directory structure subdivided by year. The "new" subdirectory contain plots at a higher resolution but currently are not available for dates early in the mission. These data consist of output from the SWAVES HFR and LFR receivers. ? the High Frequency Receivers (HFR) - for spectral analysis and direction finding of radio noise generated from a few solar radii (16 MHz) to about half an Astronomical Unit (125 kHz) ? the Low Frequency Receiver (LFR) - for spectral analysis and direction finding from about half an Astronomical Unit (160 kHz) to one AU (2.5 kHz). |

28) | STEREO WAVES (SWAVES) Radio Intensity Spectra, both Ahead and Behind s/c | |||||||||||||||||
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Resource ID:spase://VWO/NumericalData/STEREO/SWAVES/DS.Combined.PT1M | ||||||||||||||||||

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The CDF file contains 1 minute averaged radio intensity data from both the Ahead and Behind s/c. A description of the STEREO/WAVES instrument is provided in: Bougeret, J.L, et al. (2008), S/WAVES: The Radio and Plasma Wave Investigation on the STEREO Mission, Space Science Reviews, 136, 487-528. The STEREO / WAVES (SWAVES) instruments provide unique and critical observations for all primary science objectives of the STEREO mission, the generation of CMEs, their evolution, and their interaction with Earth's magnetosphere. SWAVES can probe a CME from lift-off to Earth by detecting the coronal and interplanetary (IP) shock of the most powerful CMEs, providing a radial profile through spectral imaging, determining the radial velocity from ~2 RS (from center of sun) to Earth, measuring the density of the volume of the heliosphere between the sun and Earth, and measuring important in situ properties of the IP shock, magnetic cloud, and density compression in the fast solar wind stream that follows. SWAVES measures the fluctuation electric field present on three orthogonal monopole antennas mounted on the back (anti-sunward) surface of the spacecraft. Each monopole antenna unit is a 6 m long Beryllium-Copper (BeCu) ?stacer? spring. The three units deploy from a common baseplate that also accommodates the preamplifier housing. The 6 m length was chosen to put the antenna quarter-wave resonance near the top of the SWAVES HFR2 frequency band. These data consist of output from the SWAVES HFR and LFR receivers. ? the High Frequency Receivers (HFR) - for spectral analysis and direction finding of radio noise generated from a few solar radii (16 MHz) to about half an Astronomical Unit (125 kHz) ? the Low Frequency Receiver (LFR) - for spectral analysis and direction finding from about half an Astronomical Unit (160 kHz) to one AU (2.5 kHz). |

29) | San Marco-DL Neutral Density Data at 1-s or 21-s | |||||||||||||||||
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Resource ID:spase://VSPO/NumericalData/SanMarco-DL/DBI/PT1S | ||||||||||||||||||

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This total neutral density data set from the San Marco D/L satellite Drag Balance Instrument (DBI) was provided by the PI team at the Centro Ricerche Aerospaziali in Rome, Italy. It contains the 1-second DBI data for the whole San Marco mission in ASCII format on CD (originally provide on 24 floppy diskettes). Each data file (file extension .D2) contains the time and the measured total density at that time for consecutive measurements. A new file is started any time there is a data gap of more than a few seconds. A corresponding file (.D1) contains information about the exact start and stop time of the specific measurement period, about the status of all experiments and other important information for the particular orbit, e.g., the Time of the Last Maneuver; this time parameter is important to sort out dynamically perturbed periods. Two high frequency filters and a filter for the satellite spin frequency were applied to clean the density data. Regular and irregular bias patterns were computed and recorded in the D1 files. 21-second averages of these data are generated using the PI-provided software to generate orbit parameters. The data are in ASCII format and each data record includes the date, time, total density, error, altitude, latitude, longitude, and local solar time. Further details about the San Marco spacecraft, experiment, and data sets can be found at the San Marco home page, http://crpsm.psm.uniroma1.it/ |

30) | THEMIS-A: On Board moments: ESA and SST Electron/Ion moments, density, flux, velocity, pressure and temperature. | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/THEMIS/A/MOM/PT3S | ||||||||||||||||||

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THEMIS-A On Board moments. On board data outputs include number density, particle flux, energy flux, and a six component symetric momentum flux tensor. Other moments are calculated from these partial moments on the ground adding total pressure, velocity, plasma temperature (measured as a three dimensional energy vector), and a six component symetric pressure tensor to the list of data products. Number density and total pressure are scalar outputs. Velocity is calculated in DSL, GSE, GSM, and MFA coordinates (coordinate descriptions are listed below in Table 1). Magnetic Field Aligned pressure tensor and temperature are calculated as well. All quantities are calculated for both ions and electrons from a combination of ESA and SST data. Moments data are taken at spin resolution in all ESA survey modes except burst. The spacecraft potential, as measure by the EFI, is used to correct for spacecraft charging by shifting the particle energies for calculation; this eliminates contamination from photo-electrons. Also, weighting factors are used to account for instrument specific energy and angle efficiency variations. Table 1: Coordinate Descriptions. Despun Sun - L-vector (DSL): Z-axis points towards the spin axis, the Y-axis is obtained from the cross product of Z and the Spacecraft-Sun direction as viewed from the probe. The X-axis sits in the Z-axis-Sun plane and completes a right handed system. Geocentric Solar Ecliptic (GSE): Z-axis is normal to the solar ecliptic, the X-axis points from earth towards the Sun, and Y complets a right handed system. Geocentric solar Magnetosphereic (GSM): X-axis points from Earth to the Sun, the Y-axis is orthogonal to the Earth's magnetic dipole and points towards the dusk side, and the X-Z plane contains the dipole axis. Magnetic Field Aligned (MFA): Z-axis points along magnetic field lines, the Y-axis is the orthonormal cross product of the Z-axis and a vector pointing towards the Sun, and the X-axis completes the right handed system. |

31) | THEMIS-B: On Board moments: ESA and SST Electron/Ion moments, density, flux, velocity, pressure and temperature. | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/THEMIS/B/MOM/PT3S | ||||||||||||||||||

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THEMIS-B On Board moments. On board data outputs include number density, particle flux, energy flux, and a six component symetric momentum flux tensor. Other moments are calculated from these partial moments on the ground adding total pressure, velocity, plasma temperature (measured as a three dimensional energy vector), and a six component symetric pressure tensor to the list of data products. Number density and total pressure are scalar outputs. Velocity is calculated in DSL, GSE, GSM, and MFA coordinates (coordinate descriptions are listed below in Table 1). Magnetic Field Aligned pressure tensor and temperature are calculated as well. All quantities are calculated for both ions and electrons from a combination of ESA and SST data. Moments data are taken at spin resolution in all ESA survey modes except burst. The spacecraft potential, as measure by the EFI, is used to correct for spacecraft charging by shifting the particle energies for calculation; this eliminates contamination from photo-electrons. Also, weighting factors are used to account for instrument specific energy and angle efficiency variations. Table 1: Coordinate Descriptions. Despun Sun - L-vector (DSL): Z-axis points towards the spin axis, the Y-axis is obtained from the cross product of Z and the Spacecraft-Sun direction as viewed from the probe. The X-axis sits in the Z-axis-Sun plane and completes a right handed system. Geocentric Solar Ecliptic (GSE): Z-axis is normal to the solar ecliptic, the X-axis points from earth towards the Sun, and Y complets a right handed system. Geocentric solar Magnetosphereic (GSM): X-axis points from Earth to the Sun, the Y-axis is orthogonal to the Earth's magnetic dipole and points towards the dusk side, and the X-Z plane contains the dipole axis. Magnetic Field Aligned (MFA): Z-axis points along magnetic field lines, the Y-axis is the orthonormal cross product of the Z-axis and a vector pointing towards the Sun, and the X-axis completes the right handed system. |

32) | THEMIS-D: On Board moments: ESA and SST Electron/Ion moments, density, flux, velocity, pressure and temperature. | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/THEMIS/D/MOM/PT3S | ||||||||||||||||||

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THEMIS-D On Board moments. On board data outputs include number density, particle flux, energy flux, and a six component symetric momentum flux tensor. Other moments are calculated from these partial moments on the ground adding total pressure, velocity, plasma temperature (measured as a three dimensional energy vector), and a six component symetric pressure tensor to the list of data products. Number density and total pressure are scalar outputs. Velocity is calculated in DSL, GSE, GSM, and MFA coordinates (coordinate descriptions are listed below in Table 1). Magnetic Field Aligned pressure tensor and temperature are calculated as well. All quantities are calculated for both ions and electrons from a combination of ESA and SST data. Moments data are taken at spin resolution in all ESA survey modes except burst. The spacecraft potential, as measure by the EFI, is used to correct for spacecraft charging by shifting the particle energies for calculation; this eliminates contamination from photo-electrons. Also, weighting factors are used to account for instrument specific energy and angle efficiency variations. Table 1: Coordinate Descriptions. Despun Sun - L-vector (DSL): Z-axis points towards the spin axis, the Y-axis is obtained from the cross product of Z and the Spacecraft-Sun direction as viewed from the probe. The X-axis sits in the Z-axis-Sun plane and completes a right handed system. Geocentric Solar Ecliptic (GSE): Z-axis is normal to the solar ecliptic, the X-axis points from earth towards the Sun, and Y complets a right handed system. Geocentric solar Magnetosphereic (GSM): X-axis points from Earth to the Sun, the Y-axis is orthogonal to the Earth's magnetic dipole and points towards the dusk side, and the X-Z plane contains the dipole axis. Magnetic Field Aligned (MFA): Z-axis points along magnetic field lines, the Y-axis is the orthonormal cross product of the Z-axis and a vector pointing towards the Sun, and the X-axis completes the right handed system. |

33) | THEMIS-E: On Board moments: ESA and SST Electron/Ion moments, density, flux, velocity, pressure and temperature. | |||||||||||||||||
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Resource ID:spase://VMO/NumericalData/THEMIS/E/MOM/PT3S | ||||||||||||||||||

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THEMIS-E On Board moments. On board data outputs include number density, particle flux, energy flux, and a six component symetric momentum flux tensor. Other moments are calculated from these partial moments on the ground adding total pressure, velocity, plasma temperature (measured as a three dimensional energy vector), and a six component symetric pressure tensor to the list of data products. Number density and total pressure are scalar outputs. Velocity is calculated in DSL, GSE, GSM, and MFA coordinates (coordinate descriptions are listed below in Table 1). Magnetic Field Aligned pressure tensor and temperature are calculated as well. All quantities are calculated for both ions and electrons from a combination of ESA and SST data. Moments data are taken at spin resolution in all ESA survey modes except burst. The spacecraft potential, as measure by the EFI, is used to correct for spacecraft charging by shifting the particle energies for calculation; this eliminates contamination from photo-electrons. Also, weighting factors are used to account for instrument specific energy and angle efficiency variations. Table 1: Coordinate Descriptions. Despun Sun - L-vector (DSL): Z-axis points towards the spin axis, the Y-axis is obtained from the cross product of Z and the Spacecraft-Sun direction as viewed from the probe. The X-axis sits in the Z-axis-Sun plane and completes a right handed system. Geocentric Solar Ecliptic (GSE): Z-axis is normal to the solar ecliptic, the X-axis points from earth towards the Sun, and Y complets a right handed system. Geocentric solar Magnetosphereic (GSM): X-axis points from Earth to the Sun, the Y-axis is orthogonal to the Earth's magnetic dipole and points towards the dusk side, and the X-Z plane contains the dipole axis. Magnetic Field Aligned (MFA): Z-axis points along magnetic field lines, the Y-axis is the orthonormal cross product of the Z-axis and a vector pointing towards the Sun, and the X-axis completes the right handed system. |

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