Ceres internal structure from geophysical constraints

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dc.contributor.authorKing, Scott D.en
dc.contributor.authorCastillo-Rogez, Julie C.en
dc.contributor.authorToplis, M. J.en
dc.contributor.authorBland, Michael T.en
dc.contributor.authorRaymond, Carol A.en
dc.contributor.authorRussell, Christopher T.en
dc.contributor.departmentGeosciencesen
dc.date.accessioned2020-07-06T14:11:34Zen
dc.date.available2020-07-06T14:11:34Zen
dc.date.issued2018-09en
dc.description.abstractThermal evolution modeling has yielded a variety of interior structures for Ceres, ranging from a modestly differentiated interior to more advanced evolution with a dry silicate core, a hydrated silicate mantle, and a volatile-rich crust. Here we compute the mass and hydrostatic flattening from more than one hundred billion three-layer density models for Ceres and describe the characteristics of the population of density structures that are consistent with the Dawn observations. We show that the mass and hydrostatic flattening constraints from Ceres indicate the presence of a high-density core with greater than a 1 sigma probability, but provide little constraint on the density, allowing for core compositions that range from hydrous and/or anhydrous silicates to a mixture of metal and silicates. The crustal densities are consistent with surface observations of salts, water ice, carbonates, and ammoniated clays, which indicate hydrothermal alteration, partial fractionation, and the possible settling of heavy sulfide and metallic particles, which provide a potential process for increasing mass with depth.en
dc.description.adminPublic domain – authored by a U.S. government employeeen
dc.description.notesWe thank Walter Kiefer, Anton Ermakov, and an anonymous reviewer for their constructive comments. We thank Frederic Chambat for making the Matlab program based on Chambat et al. (2010) available. S. D. K. is supported by NASA award NNX15AI30G from the Dawn at Ceres Guest Investigator Program. We thank the Dawn team for the development, cruise, orbital insertion, and operations of the Dawn spacecraft at Ceres.; C. T. R. is supported by the Discovery Program through contract NNM05AA86C to the University of California, Los Angeles.; A portion of this work was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. The authors have no conflict of interest to declare.en
dc.description.sponsorshipNASA from the Dawn at Ceres Guest Investigator Program [NNX15AI30G]; Discovery ProgramAustralian Research Council [NNM05AA86C]; NASANational Aeronautics & Space Administration (NASA)en
dc.format.mimetypeapplication/pdfen
dc.identifier.doihttps://doi.org/10.1111/maps.13063en
dc.identifier.eissn1945-5100en
dc.identifier.issn1086-9379en
dc.identifier.issue9en
dc.identifier.urihttp://hdl.handle.net/10919/99271en
dc.identifier.volume53en
dc.language.isoenen
dc.rightsCreative Commons CC0 1.0 Universal Public Domain Dedicationen
dc.rights.urihttp://creativecommons.org/publicdomain/zero/1.0/en
dc.titleCeres internal structure from geophysical constraintsen
dc.title.serialMeteoritics & Planetary Scienceen
dc.typeArticle - Refereeden
dc.type.dcmitypeTexten
dc.type.dcmitypeStillImageen

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