Progress report on the ultra heavy cosmic ray experiment (AO178)

Details Progress report on the ultra heavy cosmic ray experiment (AO178) Progress report on the ultra heavy cosmic ray experiment (AO178)

Apr 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993ldef.symp..261t&link_type=abstract

In NASA. Langley Research Center, LDEF: 69 Months in Space. Part 1: Second Post-Retrieval Symposium p 261-268 (SEE N93-29621 11-

Astronomy and Astrophysics

Astrophysics

Cosmic Rays, Heavy Nuclei, Long Duration Exposure Facility, Radiation Detectors, Radiation Dosage, Thermal Analysis, Energy Spectra, Solid State Devices, Temperature Effects

Scientific paper

The Ultra Heavy Cosmic Ray Experiment (UHCRE) is based on a modular array of 192 side-viewing solid state nuclear track detector stacks. These stacks were mounted in sets of four in 48 pressure vessels employing sixteen peripheral Long Duration Exposure Facility (LDEF) trays. The extended duration of the LDEF mission has resulted in a greatly enhanced scientific yield from the UHCRE. The geometry factor for high energy cosmic ray nuclei, allowing for Earth shadowing, was 30 sq m-sr, giving a total exposure factor of 170 sq m-sr-y at an orbital inclination of 28.4 degrees. Scanning results indicate that about 3000 cosmic ray nuclei in the charge region with Z greater than 65 were collected. This sample is more than ten times the current world data in the field (taken to be the data set from the HEAO-3 mission plus that from the Ariel-6 mission) and is sufficient to provide the world's first statistically significant sample of actinide (Z greater than 88) cosmic rays. Results to date are presented including details of ultra-heavy cosmic ray nuclei, analysis of pre-flight and post-flight calibration events and details of track response in the context of detector temperature history. The integrated effect of all temperature and age related latent track variations cause a maximum charge shift of +/- 0.8 e for uranium and +/- 0.6 e for the platinum-lead group. The precision of charge assignment as a function of energy is derived and evidence for remarkably good charge resolution achieved in the UHCRE is considered. Astrophysical implications of the UHCRE charge spectrum are discussed.

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