Silicate interactions with ammonia-water fluids on early Titan

Details Silicate interactions with ammonia-water fluids on early Titan Silicate interactions with ammonia-water fluids on early Titan

Feb 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994jgr....99.3745e&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 99, no. E2, p. 3745-3752

Mathematics

Logic

20

Argon, Atmospheric Chemistry, Atmospheric Composition, Atmospheric Models, Reaction Kinetics, Satellite Atmospheres, Satellite Surfaces, Silicates, Thermodynamic Properties, Titan, Deposition, Feldspars, Gas Chromatography, Liquid Ammonia, Mass Spectrometers, Mathematical Models, Potassium, Saturn, Satellites, Titan, Silicate, Water, Ammonia, Ocean, Fluid, Surface, Thermodynamics, Model, Sodium, Potassium, Ice, Enrichment, Impact Effects, Argon 40, Calculations, Kinetics, Volcanism, Decay, Resurfacing, Solu

Scientific paper

Plausible models of the early history of Titan suggest that ammonia and water were present in liquid form at the surface. We show here by thermodynamic modeling that such an ocean could have reacted with silicates to put substantial quantities of sodium and potassium into solution. Following the formation of an ice crust by cooling, mantle ammonia-water fluids enriched in potassium would have been brought to the surface through the cryogenic equivalent of volcanism. Later impacts would have released the Ar-40 produced by decay of the K-40 into the atmosphere. The abundance of atmospheric Ar-40, measurable by the Huygens probe gas chromatograph mass spectrometer, may be dominated by this source and hence gives a proxy indication of the volume of ammonia-water resurfacing on Titan over geologic time.

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