CO2 on Titan

Details CO2 on Titan CO2 on Titan

Nov 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983jgr....88.8709s&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 88, Nov. 1, 1983, p. 8709-8715.

Astronomy and Astrophysics

Astronomy

85

Astronomical Spectroscopy, Atmospheric Composition, Carbon Dioxide Concentration, Satellite Atmospheres, Titan, Abundance, Emission Spectra, Infrared Spectra, Meteoritic Composition, Photochemical Reactions, Planetology, Steady State, Voyager 1 Spacecraft

Scientific paper

A sharp stratospheric emission feature at 667/cm in the Voyager infrared spectra of Titan is associated with the nu2 Q branch of CO2. A coupling of photochemical and radiative-transfer theory yields an average mole fraction above the 110 mbar level of (1.5 + 1.5 or - 0.8) x 10 to the -9th, with most of the uncertainty being due to imprecise knowledge of the vertical distribution. CO2 is found to be in a steady state, with its abundance being regulated principally by the 72 K cold trap near the tropopause and secondarily by the rate at which water-bearing meteoritic material enters the top of the atmosphere. An influx of water about 0.4 times that at the top of the terrestrial atmosphere is consistent with a combination of the observed CO2 abundance and a steady-state CO mole fraction of 0.00011; the thoeretical value for CO is close to the value observed by Lutz et al. (1983), although there are large margins for error in both numbers. If steady-state conditions for CO prevail, little information is available regarding the evolution of Titan's atmosphere.

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