What can we learn by comparing Earth and Titan's upper atmospheres?

Details What can we learn by comparing Earth and Titan's upper atmospheres? What can we learn by comparing Earth and Titan's upper atmospheres?

May 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agusm.u53a..04g&link_type=abstract

American Geophysical Union, Fall Meeting 2007, abstract #U53A-04

Physics

6281 Titan, 2423 Ionization Processes (7823), 2459 Planetary Ionospheres (5435, 5729, 6026), 2479 Solar Radiation And Cosmic Ray Effects

Scientific paper

The Saturnian moon, Titan, is the only moon in the Solar System to sustain a dense, permanent atmosphere. Its dominant atmospheric constituent, molecular nitrogen, is a major species in the terrestrial atmosphere. Earth and Titan also share a similar obliquity (near 25 degrees) yielding season cycle and a similar surface pressure (of the order of one bar). Bearing in mind this common basis, differences in distance from the Sun, in forcing from the magnetized environment and from below, in atmospheric composition (molecular nitrogen apart), and in gravity make a comparison of Earth and Titan's upper atmospheres a very relevant and constructive undertaking. Is Titan's atmosphere "just" colder than the present terrestrial atmosphere? We will present a quantitative comparison of Earth and Titan's upper atmospheres in the context of the Cassini/TA flyby. In particular, we will focus on the contribution of solar forcing and induced photoelectron flux to the upper atmospheres of both bodies. The contribution of various energy sources to Titan's upper atmosphere will be derived from comparison of modelling results against Cassini/CAPS plasma observations.

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