Volume 566, June 2014
|Number of page(s)||14|
|Section||Planets and planetary systems|
|Published online||27 June 2014|
A time-dependent photochemical model for Titan’s atmosphere and the origin of H2O⋆
1 Instituto de Astrofísica de Andalucía - CSIC, c/ Glorieta de la Astronomía s/n, 18008 Granada, Spain
2 LESIA, Observatoire de Paris-Meudon, 92195 Meudon Principal Cedex, France
3 Max-Planck-Institut für Sonnensystemforschung, Max-Planck-Str. 2, 37191 Katlenburg-Lindau, Germany
Received: 19 November 2013
Accepted: 17 April 2014
Context. Titan’s stratosphere contains oxygen compounds (CO, CO2, and H2O), implying an external source of oxygen whose nature is still uncertain. Recent observations from the Herschel Space Observatory using the HIFI and PACS instruments and the Cassini/CIRS, as well as steady-state photochemical modeling indicate that the amounts of CO2 and H2O in Titan’s stratosphere may imply inconsistent values of the OH/H2O input flux, and that the oxygen source is time-variable.
Aims. We attempt to reconcile the H2O and CO2 observed profiles in Titan’s atmosphere by using an updated photochemical scheme and developing several time-dependent scenarios for the influx/evolution of oxygen species.
Methods. We use a time-dependent photochemical model of Titan’s atmosphere to calculate effective lifetimes and the response of Titan’s oxygen compounds to changes in the oxygen input flux. Two variants for the C-H-O chemical network are considered. We investigate a time-variable Enceladus source and the evolution of material delivered by a cometary impact.
Results. We find that the effective lifetime of H2O in Titan’s atmosphere is only a factor of six shorter than that of CO2 and exceeds 10 yr below 200 km. A time-variable Enceladus source, involving a decrease by a factor of 5–20 in the OH/H2O flux over the last few centuries, shows promise in explaining the relative CO2/H2O profiles. However, if the previous measurements from the Herschel Space Observatory are representative of Titan’s atmospheric water, an additional H2O loss to the haze term is needed to bring the model in full agreement with the data. In an alternate situation, CO2 production following a cometary impact that occurred at least 220–300 yr ago can in principle explain the CO2 “excess” in Titan’s stratosphere, but this scenario is highly unlikely, given the estimates of the impact rate at Titan.
Key words: planets and satellites: atmospheres / planets and satellites: individual: Titan / planets and satellites: composition
Tables 1–3 are available in electronic form at http://www.aanda.org
© ESO, 2014
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