ATMOSPHERIC SPUTTERING MODEL IN THE MARTIAN, VENUS AND TITAN ENVIRONMENTS

Details ATMOSPHERIC SPUTTERING MODEL IN THE MARTIAN, VENUS AND TITAN ENVIRONMENTS ATMOSPHERIC SPUTTERING MODEL IN THE MARTIAN, VENUS AND TITAN ENVIRONMENTS

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufm.p13d..01r&link_type=abstract

American Geophysical Union, Fall Meeting 2009, abstract #P13D-01

Physics

[0325] Atmospheric Composition And Structure / Evolution Of The Atmosphere, [0328] Atmospheric Composition And Structure / Exosphere, [0343] Atmospheric Composition And Structure / Planetary Atmospheres

Scientific paper

: Atmospheric sputtering is a well-known process acting on planetary atmospheres in a similar way in which ion-sputtering acts on surfaces of airless bodies: solar energetic ions impact on the upper regions of planetary atmospheres and may cause significant escape. In particular, a collision cascade below the exobase is expected, and the yield of the process may be very high, allowing a consistent flux outward from the atmosphere. We studied the atmospheric sputtering process acting on three different bodies of the Solar System: the two planets Mars and Venus and the Saturn satellite Titan. Mars and Venus do not possess an intrinsic magnetic field; for this reason, atmospheric sputtering is expected to act more effectively on their atmospheres. Titan, which is embedded in the strong Saturnian magnetosphere for the most part of its orbit, is exposed to both magnetospheric and solar wind ion precipitation. To study this process we developed a Montecarlo single-particle. The results and comparisons are shown here.

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