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    The long-term stability of a possible aqueous ammonium sulfate ocean inside Titan

    Grindrod, Peter M. and Fortes, Andrew Dominic and Nimmo, F. and Feltham, D. and Brodholt, J.P. and Vočadlo, L. (2008) The long-term stability of a possible aqueous ammonium sulfate ocean inside Titan. Icarus 197 (1), pp. 137-151. ISSN 0019-1035.

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    We model the thermal evolution of a subsurface ocean of aqueous ammonium sulfate inside Titan using a parameterized convection scheme. The cooling and crystallization of such an ocean depends on its heat flux balance, and is governed by the pressure-dependent melting temperatures at the top and bottom of the ocean. Using recent observations and previous experimental data, we present a nominal model which predicts the thickness of the ocean throughout the evolution of Titan; after 4.5 Ga we expect an aqueous ammonium sulfate ocean 56 km thick, overlain by a thick (176 km) heterogeneous crust of methane clathrate, ice I and ammonium sulfate. Underplating of the crust by ice I will give rise to compositional diapirs that are capable of rising through the crust and providing a mechanism for cryovolcanism at the surface. We have conducted a parameter space survey to account for possible variations in the nominal model, and find that for a wide range of plausible conditions, an ocean of aqueous ammonium sulfate can survive to the present day, which is consistent with the recent observations of Titan's spin state from Cassini radar data [Lorenz, R.D., Stiles, B.W., Kirk, R.L., Allison, M.D., del Marmo, P.P., Iess, L., Lunine, J.I., Ostro, S.J., Hensley, S., 2008. Science 319, 1649–1651].


    Item Type: Article
    Keyword(s) / Subject(s): Titan, Ices, Interiors, Thermal histories, Astrobiology
    School: Birkbeck Faculties and Schools > Faculty of Science > School of Natural Sciences
    Depositing User: Administrator
    Date Deposited: 30 Sep 2013 13:08
    Last Modified: 02 Aug 2023 17:07


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