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Crystallization of a Subsurface Ocean on Triton

dc.contributor.advisorHier-Majumder, Saswataen_US
dc.contributor.authorGaeman, Jodi Sharaen_US
dc.date.accessioned2012-02-17T07:04:12Z
dc.date.available2012-02-17T07:04:12Z
dc.date.issued2011en_US
dc.identifier.urihttp://hdl.handle.net/1903/12350
dc.description.abstractPlanetary magma oceans are present throughout the Solar System in a variety of forms. Over time, these oceans pass through various evolutionary stages, influencing the dynamics of the planetary body in question. Magma ocean evolution is explored here in greater detail through a case study of a cryomagma ocean beneath the surface of Triton, Neptune's icy satellite. Triton is hypothesized to have experienced extensive tidal dissipation within its interior early during evolution. Given the influence of tidal dissipation, this study evaluates ocean sustainability using a parametrized turbulent convection model and a coupled crust-ocean evolution model. The latter model links the thermal evolution of the crust, solved as a Stefan problem, with the crystallizing multiphase ocean. Due to an evident 'tidal blanketing' effect, these models indicate that an ocean may survive around 1 billion years given Triton's present day orbit, a timescale that increases with increasing dissipation and orbital eccentricity.en_US
dc.titleCrystallization of a Subsurface Ocean on Tritonen_US
dc.typeThesisen_US
dc.contributor.publisherDigital Repository at the University of Marylanden_US
dc.contributor.publisherUniversity of Maryland (College Park, Md.)en_US
dc.contributor.departmentGeologyen_US
dc.subject.pqcontrolledGeophysicsen_US
dc.subject.pquncontrolledIcy Satellitesen_US
dc.subject.pquncontrolledInternal Structureen_US
dc.subject.pquncontrolledSubsurface Oceanen_US
dc.subject.pquncontrolledThermal Evolutionen_US
dc.subject.pquncontrolledTidal Dissipationen_US
dc.subject.pquncontrolledTritonen_US


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