Astronomy and Astrophysics – Astronomy
Scientific paper
May 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21425102j&link_type=abstract
American Astronomical Society, AAS Meeting #214, #251.02; Bulletin of the American Astronomical Society, Vol. 41, p.751
Astronomy and Astrophysics
Astronomy
Scientific paper
Solar system surfaces can be exposed to both solar UV and plasma radiation. Depending on the surface properties, the incident radiation can produce defects and chemistry, as well as desorption and sputtering. Such effects can be seen in the composition of the ambient neutrals and plasma as well as in surface reflectance spectra. Therefore, an understanding of the radiation effects is needed to interpret observations of a number of interesting planetary bodies. In this paper we will summarize the connections between models of laboratory results and telescopic and spacecraft data.
In the inner solar system, radiation-induced desorption of trace and adsorbed species has been critical for understanding observations of Mercury and the Moon. The more volatile surfaces in the outer solar are, not surprisingly, more dramatically affected by radiation processing. Stimulated desorption of alkalis is still a marker for radiation processing, but the sputtering yields for icy surfaces can be enormous.
One of the more important effects in the outer solar system is radiation-induced decomposition. For an icy body, decomposition leads to the production of H2 and O2, which, due to their volatility, can populate the ambient gas. Since hydrogen is typically lost preferentially, decomposition is often accompanied by the production of oxygen-rich molecules in the surface and, even, micro-bubbles of oxygen and ozone. Hydrogen is also lost preferentially from surfaces containing trapped ammonia, methane, hydrogen sulfide, and organics. Radiation processing of icy surfaces containing trace amounts of carbon or sulfur can form steady state amounts of oxides, hydrated-acids and refractory residues in the surface. On surfaces rich in sulfur or carbon, radiation-induced degradation produces carbon and sulfur lag deposits.
These effects will be reviewed with emphasis on the need for good models of radiation processing in order to understand observations of planetary bodies and their gaseous and plasma environments
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