The interactions of atmospheric cosmogenic radionuclides with spacecraft surfaces

Details The interactions of atmospheric cosmogenic radionuclides with spacecraft surfaces The interactions of atmospheric cosmogenic radionuclides with spacecraft surfaces

Jan 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992ldef.symp..237g&link_type=abstract

In NASA. Langley Research Center, LDEF: 69 Months in Space. First Post-Retrieval Symposium, Part 1 p 237-247 (SEE N92-23280 14-9

Other

Beryllium Isotopes, Cosmic Rays, Long Duration Exposure Facility, Mass Spectroscopy, Metal Surfaces, Spallation, Surface Reactions, Half Life, Oxygen Atoms, Protons, Teflon (Trademark), Upper Atmosphere

Scientific paper

The discovery of the cosmogenic radionuclide Be-7 on the front surface of the Long Duration Exposure Facility (LDEF) spacecraft has opened opportunities to investigate new phenomena in several disciplines of space science. The experiments performed for this work show that the Be-7 results only if the source of the isotope is the atmosphere through which the spacecraft passed. We should expect that the uptake of beryllium in such circumstances will depend on the chemical form of the Be and the chemical nature of the substrate. It was found that the observed concentration of Be-7 does, in fact, differ between metal surfaces and organic surfaces such as PTFE (teflon). It is noted, however, that: (1) organic surfaces, even PTFE, are etched by the atomic oxygen found under these orbital conditions, and (2) the relative velocity of the species is 8 km-1s relative to the surface and the interaction chemistry and physics may differ from the norm. The Be-7 is formed by spallation of O and N nuclei under cosmic ray proton bombardment. The principal source region is at altitudes of 12-15 km. While very small quantities are produced above 300 km, the amount measured on the LDEF was 3 to 4 orders of magnitude higher than expected from production at orbital altitude. The most reasonable explanation is that Be-7 is rapidly transported from low altitudes by some unknown mechanism. The process must take place on a time scale similar to the half-life of the isotope (53 days). Many other isotopes are produced by cosmic ray reactions, and some of these are suited to measurement by the extremely sensitive methods of accelerator mass spectrometry. A program was initiated to search for these isotopes and it is hoped that such studies will provide new methods for studying mixing in the upper atmosphere.

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