This page summarizes information about the selected resource and its origin based on SPASE metadata.
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12sec-averaged sectored count rates from CA60 - Channels W1, W2, W3, W4, W5, W6, W7, and W8.
The HISCALE instrument contains the Low-Energy Magnetic Spectrometers (LEMS), the Low-Energy Foil Spectrometers (LEFS) and the Composition Aperture (CA). There is a LEMS detector at 30 degrees from the spacecraft spin axis and a second at 120 degrees. LEFS is positioned at 60 degrees from the spacecraft spin axis with a second LEFS detector at 150 degrees. The CA detector is positioned at 60 degrees from the spacecraft spin axis. The parameter descriptions of this document reference the detectors by their acronyms and angle from the spacecraft spin axis, i.e. LEMS30, LEMS120, LEFS60, LEFS150, and CA60.
A table summarizing the contents of HISCALE data available via the VHO/VEPO
Thomas P. Armstrong, Fundamental Technologies LLC
| Role | Person | |
|---|---|---|
| 1. | Data producer | Dr. Thomas P. Armstrong |
Folder containing zipped data files.
Thomas P. Armstrong, Fundamental Technologies LLC
Time for the record given in year, day of year, hour, min, and decimal seconds. The given time represents the beginning of the averaging interval.
| Index | Name | Valid min | Valid max | Fill value |
|---|---|---|---|---|
| 1 | Year | 1991 | 2008 | -9999 |
| 2 | Day of year | 1 | 366 | -999 |
| 3 | Hour of day | 0 | 23 | -99 |
| 4 | Minute of hour | 0 | 59 | -99 |
| 5 | Seconds of minute | 0.00 | 59.99 | -99.99 |
12sec CA60 W1 Sector 1 proton count rates between 480 and 966 keV
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W1 Sector 2 proton count rates between 480 and 966 keV
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W1 Sector 3 proton count rates between 480 and 966 keV
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W1 Sector 4 proton count rates between 480 and 966 keV
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W1 Sector 5 proton count rates between 480 and 966 keV
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W1 Sector 6 proton count rates between 480 and 966 keV
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W1 Sector 7 proton count rates between 480 and 966 keV
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W1 Sector 8 proton count rates between 480 and 966 keV
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W2 Sector 1 proton count rates between 968 and 1204 keV
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W2 Sector 2 proton count rates between 968 and 1204 keV
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W2 Sector 3 proton count rates between 968 and 1204 keV
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W2 Sector 4 proton count rates between 968 and 1204 keV
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W2 Sector 5 proton count rates between 968 and 1204 keV
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W2 Sector 6 proton count rates between 968 and 1204 keV
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W2 Sector 7 proton count rates between 968 and 1204 keV
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W2 Sector 8 proton count rates between 968 and 1204 keV
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W3 Sector 1 alpha count rates between 389 and 1278 keV/nuc
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W3 Sector 2 alpha count rates between 389 and 1278 keV/nuc
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W3 Sector 3 alpha count rates between 389 and 1278 keV/nuc
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W3 Sector 4 alpha count rates between 389 and 1278 keV/nuc
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W3 Sector 5 alpha count rates between 389 and 1278 keV/nuc
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W3 Sector 6 alpha count rates between 389 and 1278 keV/nuc
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W3 Sector 7 alpha count rates between 389 and 1278 keV/nuc
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W3 Sector 8 alpha count rates between 389 and 1278 keV/nuc
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W4 Sector 1 alpha count rates between 1277 and 6984 keV/nuc
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W4 Sector 2 alpha count rates between 1277 and 6984 keV/nuc
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W4 Sector 3 alpha count rates between 1277 and 6984 keV/nuc
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W4 Sector 4 alpha count rates between 1277 and 6984 keV/nuc
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W4 Sector 5 alpha count rates between 1277 and 6984 keV/nuc
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W4 Sector 6 alpha count rates between 1277 and 6984 keV/nuc
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W4 Sector 7 alpha count rates between 1277 and 6984 keV/nuc
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W4 Sector 8 alpha count rates between 1277 and 6984 keV/nuc
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W5 Sector 1 5.le.Z.le.12 count rates between 465 and 1709 keV/nuc
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W5 Sector 2 5.le.Z.le.12 count rates between 465 and 1709 keV/nuc
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W5 Sector 3 5.le.Z.le.12 count rates between 465 and 1709 keV/nuc
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W5 Sector 4 5.le.Z.le.12 count rates between 465 and 1709 keV/nuc
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W5 Sector 5 5.le.Z.le.12 count rates between 465 and 1709 keV/nuc
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W5 Sector 6 5.le.Z.le.12 count rates between 465 and 1709 keV/nuc
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W5 Sector 7 5.le.Z.le.12 count rates between 465 and 1709 keV/nuc
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W5 Sector 8 5.le.Z.le.12 count rates between 465 and 1709 keV/nuc
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W6 Sector 1 Z.ge.5 count rates between 1709 and 19107 keV/nuc
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W6 Sector 2 Z.ge.5 count rates between 1709 and 19107 keV/nuc
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W6 Sector 3 Z.ge.5 count rates between 1709 and 19107 keV/nuc
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W6 Sector 4 Z.ge.5 count rates between 1709 and 19107 keV/nuc
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W6 Sector 5 Z.ge.5 count rates between 1709 and 19107 keV/nuc
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W6 Sector 6 Z.ge.5 count rates between 1709 and 19107 keV/nuc
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W6 Sector 7 Z.ge.5 count rates between 1709 and 19107 keV/nuc
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W6 Sector 8 Z.ge.5 count rates between 1709 and 19107 keV/nuc
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W7 Sector 1 Z.ge.12 count rates between 239 and 840 keV/nuc
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W7 Sector 2 Z.ge.12 count rates between 239 and 840 keV/nuc
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W7 Sector 3 Z.ge.12 count rates between 239 and 840 keV/nuc
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W7 Sector 4 Z.ge.12 count rates between 239 and 840 keV/nuc
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W7 Sector 5 Z.ge.12 count rates between 239 and 840 keV/nuc
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W7 Sector 6 Z.ge.12 count rates between 239 and 840 keV/nuc
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W7 Sector 7 Z.ge.12 count rates between 239 and 840 keV/nuc
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W7 Sector 8 Z.ge.12 count rates between 239 and 840 keV/nuc
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W8 Sector 1 Z.ge.12 count rates between 840 and 92663 keV/nuc
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W8 Sector 2 Z.ge.12 count rates between 840 and 92663 keV/nuc
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W8 Sector 3 Z.ge.12 count rates between 840 and 92663 keV/nuc
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W8 Sector 4 Z.ge.12 count rates between 840 and 92663 keV/nuc
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W8 Sector 5 Z.ge.12 count rates between 840 and 92663 keV/nuc
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W8 Sector 6 Z.ge.12 count rates between 840 and 92663 keV/nuc
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W8 Sector 7 Z.ge.12 count rates between 840 and 92663 keV/nuc
Geometric Factor = 0.103 cm^2-sr
12sec CA60 W8 Sector 8 Z.ge.12 count rates between 840 and 92663 keV/nuc
Geometric Factor = 0.103 cm^2-sr
X-Component of the Magnetic Field in HEE Coordinates
Y-Component of the Magnetic Field in HEE Coordinates
Z-Component of the Magnetic Field in HEE Coordinates
Magnitude of the Magnetic Field in HEE Coordinates
SPASE version 2.0.0
The objectives of this investigation are (1) to investigate the solar-flare process with measurements of non-relativistic and relativistic electrons, and non-relativistic ions, and their dependence on heliolatitude; (2) to investigate solar elemental abundances with measurements of chemical composition of nuclei of solar origin at all heliolatitudes; (3) to investigate the interplanetary propagation of solar energetic particles by measurement of anisotropy and composition parameters; (4) to investigate acceleration processes; and (5) to investigate temporal and spatial variations of particle intensity in and near the Jovian magnetosphere. The instrumentation consists of two double-ended solid state detector systems which measure ions in the range 50 keV to 5 MeV and electrons in the range 30 to 300 keV, and a (dE/dX, E) telescope using a 5-micrometer-thick front detector for ion elemental abundances in the range 1 to 15 MeV/nucleon (Fe). Each double-ended system is composed on one end of a foil spectrometer in which a 0.35 mg/sq cm thin foil excludes ions below 0.350 keV, allowing electrons above 30 keV to be detected. Further, one of the other ends of one of the systems is a magnetic spectrometer, using a rare-earth magnet to separate electrons from ions (geometric factor for ions is approximately 0.5 sq cm-sr, and for electrons 0.05 sq cm-sr). Orientation of the sensor systems is such that complete pitch-angle coverage is obtained. The instrument has a mass of 5.8 kg including shielding, and uses 4.0 W of power. The data rate is 80 bps in cruise mode and 160 bps in tracking mode. "The Heliosphere Instrument for Spectra, Composition, and Anisotropy at Low Energies (HI-SCALE) is designed to make measurements of interplanetary ions and electrons throughout the entire Ulysses mission. This ions (Ei > 50 keV) and electrons ( Ee > 30 keV ) are identified uniquely and detected by five separate solid-state detector telescopes that are oriented to give nearly complete pitch-angle coverage (i.e., coverage of essentially 4 pi ster) from the spinning spacecraft. Ion elemental abundances are determined by a delta E vs E telescope using a thin (5 micron) front solid state detector element in a three-element telescope. Expirement operation is controlled by a microprocessor-based data system. Inflight calibration is provided by radioactive sources mounted on telescope covers which can be closed for calibration purposes and for radiation protection during the course of the mission. Ion nd electron spectral information is determined using both broad-energy-range rate channels and a 32 channel pulse-height analyser (channels spaced logarithmically) for more detailed spectra. The instrument weighs 5.775 kg and uses 4.0 W of power. Some initial in-ecliptic measurements are presented which demonstrate the features of the instrument". (quote of Abstract: L. Lanzerotti et al., Astron. Astrophys. Suppl. Ser. 92, 349-363, 1992). The HISCALE instrument utilizes five separate detector systems within two mechanical structures. These systems are referenced by their name and angle with respect to the Ulysses spin axis. The systems are the Low-Energy Magnetic Spectrometer (LEMS), the Low-Energy Foil Spectrometer (LEFS) and the Composition Aperature (CA). The LEMS/LEFS systems provide pulse-height-analyzed single-detector measurements with active anticoincidence. The CA system uses a multiparameter detection technique to provide measurement of ion composition in an energy range similar to those of LEMS/LEFS.
Primary website for the Ulysses-HISCALE experiment.
Detailed description and illustrations of the HISCALE detector systems.
| Role | Person | |
|---|---|---|
| 1. | Principal investigator | Dr. Louis J. Lanzerotti |
SPASE version 2.0.0
The primary objectives of Ulysses, formerly the International Solar Polar Mission (ISPM), are to investigate, as a function of solar latitude, the properties of the solar wind and the interplanetary magnetic field, of galactic cosmic rays and neutral interstellar gas, and to study energetic particle composition and acceleration. The 55 kg payload includes two magnetometers, two solar wind plasma instruments, a unified radio/plasma wave instrument, three energetic charged particle instruments, an interstellar neutral gas sensor, a solar X-ray/cosmic gamma-ray burst detector, and a cosmic dust sensor. The communications systems is also used to study the solar corona and to search for gravitational waves. Secondary objectives included interplanetary and planetary physics investigations during the initial Earth-Jupiter phase and investigations in the Jovian magnetosphere. The spacecraft used a Jupiter swingby in Feb. 1992 to transfer to a heliospheric orbit with high heliocentric inclination, and will pass over the rotational south pole of the sun in mid-1994 at 2 AU, and over the north pole in mid-1995. A second solar orbit will take Ulysses again over the south and north poles in years 2000 and 2001, respectively. The spacecraft is powered by a single radio-isotope generator. It is spin stabilized at a rate of 5 rpm and its high-gain antenna points continuously to the earth. A nutation anomaly after launch was controlled by CONSCAN. The original mission planned for two spacecraft, one built by ESA and the other by NASA. NASA cancelled its spacecraft in 1981.
JPL's primary website for the Ulysses mission. Links to all of the experiment subpages exist here.
| Role | Person | |
|---|---|---|
| 1. | Project scientist | Dr. Edward J. Smith |
| 2. | Project scientist | Dr. Richard G. Marsden |
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