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artist concept of Ulysses spacecraft
Credit: NASA

* Mission Overview

The Ulysses mission is a joint mission with NASA and ESA to explore the solar environment at high ecliptic latitudes. It was launched 6 October 1990, and reached Jupiter for its "gravitational slingshot" in February 1992. It passed the south solar pole in June 1994 and crossed the ecliptic equator in February 1995. In addition to its solar environment instruments, Ulysses also carries plasma instruments to study the interstellar and Jovian regions, as well as two instruments for studying X-rays and gamma-rays of both solar and cosmic origins.

The Ulysses spacecraft can operate in 4 different telemetry modes: 128, 256, 512, and 1024 b/s. The time resolution of the gamma-ray burst instrument varies with the spacecraft data rate. The maximum telemetry allocation for the instrument is 40 b/s.

* Instrumentation

The Ulysses solar X-ray and cosmic gamma-ray burst experiment (GRB) has 3 main objectives: study and monitor solar flares, detect and localize cosmic gamma-ray bursts, and in-situ detection of Jovian aurorae. Ulysses is the first satellite carrying a gamma burst detector which went outside the orbit of Mars. This results in a triangulation baseline of unprecedented length, thus allowing major improvements in burst localization accuracy. The instrument was turned on 9 November 1990. GRB consists of 2 CsI scintillators (called the Hard X-ray detectors)and 2 Si surface barrier detectors (called the Soft X-ray detectors). The detectors are mounted on a ~3-m boom to reduce background generated by the spacecraft's radioisotope thermoelectric generator.

The hard X-ray detectors operate in the range 15-150 keV. The detectors consist of 2 3-mm thick x 51-mm diameter CsI(Tl) crystals mounted via plastic light tubes to photomultipliers. The hard detector changes its operating mode depending on (1) measured count rate, (2) ground command, or (3) change in spacecraft telemetry mode. The trigger level is generally set for 8-sigma above background and the sensitivity is ~1e-6 erg/cm2. When a burst trigger is recorded, the instrument switches to record high resolution data, recording it to a 32-kbit memory for a slow telemetry read out. Burst data consist of either 16 s of 8-ms resolution count rates or 64 s of 32-ms count rates from the sum of the 2 detectors. There are also 16 channel energy spectra from the sum of the 2 detectors (taken either in 1,2,4,16,or 32 second integrations). During 'wait' mode, the data are taken either in 0.25 or 0.5 s integrations and 4 energy channels (with shortest integration time being 8 s). Again, the outputs of the 2 detectors are summed.

The soft X-ray detectors consist of 2 500-micron thick x 0.5 cm2 area Si surface barrier detectors. A 100 mg/cm2 beryllium foil front window rejects the low energy X-rays and defines a conical field of view of 75 degrees (half- angle). These detectors are passively cooled and operate in the temperature range -35 to -55 degrees Celsius. This detector has 6 energy channels, covering the range 5-20 keV.

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Imagine the Universe! is a service of the High Energy Astrophysics Science Archive Research Center (HEASARC), Dr. Alan Smale (Director), within the Astrophysics Science Division (ASD) at NASA's Goddard Space Flight Center.

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Project Leader: Dr. Barbara Mattson
Curator: Meredith Gibb
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This page last updated: Tuesday, 02-Oct-2007 12:55:09 EDT