Analysis of Titan CH 4 3.3 μm upper atmospheric emission as measured by Cassini/VIMS

Details Analysis of Titan CH 4 3.3 μm upper atmospheric emission as measured by Cassini/VIMS Analysis of Titan CH 4 3.3 μm upper atmospheric emission as measured by Cassini/VIMS

Aug 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011icar..214..571g&link_type=abstract

Icarus, Volume 214, Issue 2, p. 571-583.

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Scientific paper

Sophisticated model calculating Titan's non-LTE population of CH 4 vibrational levels. Solar radiation, CH 4 -N 2 collisions, and ν 4 -quanta exchange are the relevant processes. Emission from ν 3 and ν 3 + ν 4 dominate Titan's upper atmosphere 3.3 μm limb radiance. Other weaker CH 4 bands may contribute up to 20-25% to the total limb radiance. Retrieved CH 4 abundance from Cassini-VIMS support well mixed values up to 1000 km.

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