The evolution of the atmosphere and surface of Titan from Cassini infrared observations
Flasar, F. M.
Rodriguez, S.
Stephan, K.
Bampasidis, G.
Achterberg, R.
Jaumann, R.
Lavvas, P.
Coustenis, A.
Le Mouelic,S.
Hirtzig, M.
Drossart, P.
Vinatier, S.
Jennings, D.
Nixon, C.
Teanby, N.
Solomonidou, A.
Bratsolis, E.
Saturn’s Earth-like satellite Titan has a thick and dense atmosphere consisting of nitrogen (98.4%), methane (1.6%) and trace gases such as hydrocarbons and nitriles [1]. The condensed organics are deposited on the surface and the atmosphere-surface-interior interactions shape the ground. In particular, Titan’s methane cycle, similarly to the Earth’s hydrologic cycle, plays an important role in these exchanges by transporting methane at all layers. By applying our radiative transfer code (ARTT) to Cassini/CIRS data taken during Titan flybys from 2004-2010 and to the 1980 Voyager 1 flyby values inferred from the reanalysis of the Infrared Radiometer Spectrometer (IRIS) spectra, as well as to the intervening ground- and space- based observations (such as with ISO), we study the stratospheric evolution over a Titanian year (V1 encounter Ls=9° was reached in mid-2010).
