Ceres' Broad-Scale Surface Geomorphology Largely Due To Asymmetric Internal Convection

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dc.contributor.authorKing, Scott D.en
dc.contributor.authorBland, Michael T.en
dc.contributor.authorMarchi, Simoneen
dc.contributor.authorRaymond, Carol A.en
dc.contributor.authorRussell, Christopher T.en
dc.contributor.authorScully, Jennifer E. C.en
dc.contributor.authorSizemore, Hanna G.en
dc.date.accessioned2022-06-09T13:05:41Zen
dc.date.available2022-06-09T13:05:41Zen
dc.date.issued2022-06en
dc.description.abstractWhile we now know much about the volatile-rich world of Ceres from the Dawn mission, the deep interior remains something of an enigma, shrouded by a crust composed of water ice, carbonates, phyllosilicates, salts and clathrate hydrates. While smaller than most active moons or planets, Ceres has many features commonly associated with active, icy bodies including: hydrothermal, cryovolcanic, and tectonic features. Yet on active icy moons tidal heating is a significant component of the thermal budget; it is unclear whether radiogenic heating alone would be sufficient to supply the heat necessary for Ceres' interior to undergo solid-state convection. Here we show that transient asymmetric convection develops as the temperature within the body rises from heat generated by the decay of long-lived radionuclides (e.g., U, Th, K). The onset of transient asymmetric convection may reconcile a number of puzzling features on Ceres including: the missing large craters, Hanami Planum-the region of thickened crust, the gravity and crustal thickness, and the lithospheric stress state represented by the Samhain Catenae. Hemispheric-scale instabilities may also be important in the evolution of small bodies with small cores throughout the solar system, including the small icy moons of Saturn and Uranus as well as Kuiper belt objects.en
dc.description.notesWe thank Shijie Zhong, Mike Sori, and an anonymous reviewer for thoughtful and constructive reviews. We thank the Dawn Flight Team at JPL for the development, cruise, orbital insertion, and operations of the Dawn spacecraft at Ceres. We thank the instrument teams at the Max Planck Institute, German Aerospace Center (DLR), Italian National Institute for Astrophysics (INAF), and Planetary Science Institute (PSI) for the acquisition and processing of Dawn data. We thank both of the reviewers for their helpful comments. S.D.K. is supported by NASA award NNX15AI30G from the Dawn at Ceres Guest Investigator Program. Part of the research was carried out at the Jet Propulsion Laboratory (JPL), California Institute of Technology, under a contract with the National Aeronautics and Space Administration.en
dc.description.sponsorshipNASA [NNX15AI30G]; National Aeronautics and Space Administrationen
dc.description.versionPublished versionen
dc.format.mimetypeapplication/pdfen
dc.identifier.doihttps://doi.org/10.1029/2021AV000571en
dc.identifier.eissn2576-604Xen
dc.identifier.issue3en
dc.identifier.othere2021AV000571en
dc.identifier.urihttp://hdl.handle.net/10919/110514en
dc.identifier.volume3en
dc.language.isoenen
dc.publisherAmerican Geophysical Unionen
dc.rightsCreative Commons Attribution 4.0 Internationalen
dc.rights.urihttp://creativecommons.org/licenses/by/4.0/en
dc.subjectCeresen
dc.subjectmantle convectionen
dc.subjectHanami Planumen
dc.subjecticy bodiesen
dc.titleCeres' Broad-Scale Surface Geomorphology Largely Due To Asymmetric Internal Convectionen
dc.title.serialAGU Advancesen
dc.typeArticle - Refereeden
dc.type.dcmitypeTexten

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