This data set contains raw Radio Occultation (ROCC) Original Data Records data from the Ulysses (ULY) Solar Corona Experiment (SCE) obtained during the ULY Jupiter flyby. The data target the Io Plasma Torus (IPT) and cover the period 1992-02-03 11:20 to 1992-02-09 20:46.

This data set contains raw radio tracking data from the Ulysses (ULY) Solar Corona Experiment (SCE) obtained during the ULY Jupiter flyby. The data target the Io Plasma Torus (IPT) and cover the period 1992-02-04 20:28 to 1992-02-09 15:44.

This data set contains raw radio tracking data from the Ulysses (ULY) Solar Corona Experiment (SCE) obtained during the ULY Jupiter flyby. The data target the Io Plasma Torus (IPT) and cover the period 1992-02-04 20:28 to 1992-02-09 15:44.

This data set contains ion flux data recorded by the COSPIN High Flux Telescope (HFT) during the Ulysses Jupiter encounter 1992-Jan-25 to 1992-Feb-18

This data set contains ion flux data recorded by the COSPIN High Flux Telescope (HFT) during the Ulysses Jupiter encounter 1992-Jan-25 to 1992-Feb-18.

This data set contains Ulysses ephemeris data near Jupiter covering the dates 1992-01-25 to 1992-02-18. Two slightly different versions of these data are included. The first (TRJ25_48.TAB), provided by the Ulysses MAG team (Imperial College/JPL), includes position data in Sys 3 spherical, ECL50 spherical, and ECL50 Cartesian coordinates. The Ulysses spin axis position is also provided in ECL50 spherical coordinates. The second version (SPK25_48.TAB), generated at the PDS/PPI node (UCLA), includes Sys 3 spherical trajectory, plus a spacecraft local time. Note that the position values for these two versions differ slightly. This variation is due to differences in the definitions of the Jovian physical constants used to generate them.

This data set contains Ulysses ephemeris data near Jupiter covering the dates 1992-01-25 to 1992-02-18. Two slightly different versions of these data are included. The first (TRJ25_48.TAB), provided by the Ulysses MAG team (Imperial College/JPL), includes position data in Sys 3 spherical, ECL50 spherical, and ECL50 Cartesian coordinates. The Ulysses spin axis position is also provided in ECL50 spherical coordinates. The second version (SPK25_48.TAB), generated at the PDS/PPI node (UCLA), includes Sys 3 spherical trajectory, plus a spacecraft local time. Note that the position values for these two versions differ slightly. This variation is due to differences in the definitions of the Jovian physical constants used to generate them.

The Ulysses spacecraft was occulted by the Io Plasma Torus (IPT) during its Jupiter encounter on 8 February 1992. The Ulysses dual-frequency radio subsystem used by the Ulysses Solar Corona Experiment (SCE) was utilized to measure the electron content (column density) of the IPT [BIRDETAL1992B]. In the nominal mode for radio-sounding observations [BIRDETAL1992A], both downlinks (S-band: f_s = 2.3 GHz X-band: f_x = 8.4 GHz) are phase coherent with the uplink (S-band: f_u = 2.1 GHz). The dual-frequency radio-sounding technique exploits the dispersive nature of ionized media on the propagation of the two downlinks. The tiny Doppler shift due to plasma moving in and out of the ray path is greater at S-band than at the higher frequency X-band.

The Ulysses spacecraft was occulted by the Io Plasma Torus (IPT) during its Jupiter encounter on 8 February 1992. The Ulysses dual-frequency radio subsystem used by the Ulysses Solar Corona Experiment (SCE) was utilized to measure the electron content (column density) of the IPT. In the nominal mode for radio-sounding observations, both downlinks (S-band: f_s = 2.3 GHz X-band: f_x = 8.4 GHz) are phase coherent with the uplink (S-band: f_u = 2.1 GHz). The dual-frequency radio-sounding technique exploits the dispersive nature of ionized media on the propagation of the two downlinks. The tiny Doppler shift due to plasma moving in and out of the ray path is greater at S-band than at the higher frequency X-band.

The archived data consist of count rates from the sum of two hemispherical detectors covering 4 pi steradians and operating continuously. The detectors are 3 mm thick CsI scintillators coupled to photomultiplier tubes. The nominal energy range is 25-150 keV, but the below table should be consulted to find the accurate thresholds for any day of the mission. A more complete description of the instrument may be found in [HURLEYETAL1992] and [COTINETAL1983]. Although the prime objectives of this investigation are the study of solar and cosmic x- and gamma-ray bursts, it should be noted that the experiment is also sensitive to solar protons and electrons. The former deposit energy directly in the scintillator if they are energetic enough, while the latter may produce x- radiation locally by bremsstrahlung. Thus although the counting rates are generally stable at about 500 c/s over the long term, there are periods of weeks to a month or so when the rates increase considerably due to particles. Examples may be found in March 1991 (solar protons) and February 1992 (particles in the Jovian magnetosphere). The time resolution of the data takes on one of four values depending on the telemetry rate and instrument operating mode: 0.25, 0.5, 1, or 2 seconds.