High-pressure experiments on the stability of methane hydrates in the H2O-NH3-CH4 system with applications to Titan's cryovolcanism.

Details High-pressure experiments on the stability of methane hydrates in the H2O-NH3-CH4 system with applications to Titan's cryovolcanism. High-pressure experiments on the stability of methane hydrates in the H2O-NH3-CH4 system with applications to Titan's cryovolcanism.

Aug 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007epsc.conf..887c&link_type=abstract

European Planetary Science Congress 2007, Proceedings of a conference held 20-24 August, 2007 in Potsdam, Germany. Online at ht

Astronomy and Astrophysics

Astrophysics

Scientific paper

The current methane abundance in Titan's thick atmosphere cannot be explained without the existence of replenishment processes. Indeed, the intense photochemistry taking place in the atmosphere would destroy the 2-5% CH4 amounts measured by the GCMS onboard the Huygens probe [1] within 10-100 Myr [e.g. 2]. Among the several hypotheses that could explain this replenishment, release of methane during cryovolcanic events seems highly likely. The VIMS [3] and Radar instruments [4] onboard the Cassini spacecraft have brought substantial evidence for cryovolcanic features on Titan's surface. A numerical model has shown the possibility to release CH4 by dissociating methane clathrate hydrates at depth, due to interaction of a clathrate layer with warm ice intrusions [5]. However, the effect of volatile compounds, dissolved (e.g. N2) or in solution (e.g. NH3), would most certainly play a major role in cryovolcanic processes. High-pressure low-temperature experimental investigations on the effect of ammonia on methane hydrates' dissociation are conducted within an optical sapphire-anvil cell. Preliminary results have been previously presented, which lead to contradictory interpretations so far [6,7]. As further experiments are being performed, the reliability of the experimental measurements and the reasons for observing discrepancies in the results can be adressed with more and more confidence. This poster will discuss the experimental issues encountered in the H2O-NH3-CH4 system, up-todate experimental results, as well as their implications for Titan's cryovolcanism. References: [1] Niemann HB et al., Nature 438, 779-784 (2005). [2] Yung YL et al., Astrophys. J. Suppl., 55, 465-506 (1984). [3] Sotin C et al., Nature 435, 786-789 (2005). [4] Lopes RMC et al., Icarus 186, 395-412 (2007). [5] Tobie G et al., Nature 440 (2), 61-64 (2006). [6] Choukroun M et al., 37th Lunar and Planet. Sci. Conf. Abstract #1640 (2006). [7] Choukroun M et al., 38th Lunar and Planet. Sci. Conf. Abstract #1606 (2007).

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