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Conference Papers Year : 2008

Sequestration of ethane in the cryovolcanic subsurface of Titan

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Abstract

Saturn's largest satellite, Titan, has a thick atmosphere dominated by nitrogen and methane. The dense orange-brown smog hiding the satellite's surface is produced by photochemical reactions of methane, nitrogen and their dissociation products with solar ultraviolet, which lead primarily to the formation of ethane and heavier hydrocarbons. In the years prior to the exploration of Titan's surface by the Cassini-Huygens spacecraft, the production and condensation of ethane was expected to have formed a satellite-wide ocean one kilometer in depth, assuming that it was generated over the Solar system's lifetime. However, Cassini-Huygens observations failed to find any evidence of such an ocean. Here we describe the main cause of the ethane deficiency on Titan: cryovolcanic lavas regularly cover its surface, leading to the percolation of the liquid hydrocarbons through this porous material and its accumulation in subsurface layers built up during successive methane outgassing events. The liquid stored in the pores may, combined with the ice layers, form a stable ethane-rich clathrate reservoir, potentially isolated from the surface.
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Dates and versions

insu-00361731 , version 1 (16-02-2009)

Identifiers

  • HAL Id : insu-00361731 , version 1

Cite

Olivier Mousis, Bernard Schmitt. Sequestration of ethane in the cryovolcanic subsurface of Titan. SF2A-2008 : Proceedings of the Annual meeting of the French Society of Astronomy and Astrophysics, Jul 2008, Paris, France. pp.429. ⟨insu-00361731⟩
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