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dc.contributor.authorBierson, C. J.
dc.contributor.authorPhillips, Roger J.
dc.contributor.authorNimmo, Francis
dc.contributor.authorBesserer, Jonathan
dc.contributor.authorMilbury, Colleen
dc.contributor.authorKeane, James T.
dc.contributor.authorSoderblom, Jason M.
dc.contributor.authorZuber, Maria T.
dc.date.accessioned2017-02-08T19:00:18Z
dc.date.available2017-02-08T19:00:18Z
dc.date.issued2016-08
dc.identifier.citationInteractions between complex craters and the lunar crust: Analysis using GRAIL data 2016, 121 (8):1488 Journal of Geophysical Research: Planetsen
dc.identifier.issn21699097
dc.identifier.doi10.1002/2016JE005090
dc.identifier.urihttp://hdl.handle.net/10150/622471
dc.description.abstractA high-resolution gravity map over the entire lunar surface has been derived from data acquired by the Gravity Recovery and Interior Laboratory (GRAIL) mission. Soderblom et al. (2015) showed that crater Bouguer gravity anomalies scale with crater diameter and porosity for craters in the lunar highlands. Here we extend this study globally, examining complex craters in each of the three lunar terranes: highlands, maria, and the South Pole-Aitken basin. We find that craters within South Pole-Aitken basin and in the lunar maria have statistically different Bouguer anomalies from those in the lunar highlands. These differences are best explained by differences in crustal porosity among the three terranes. Though there is still much unresolved scatter in the data, we find that no other lunar material properties (crustal thickness, density gradient, etc.) are able to improve our model fit to the data.
dc.description.sponsorshipGRAIL project; NASA [NNX15AP90G, NNX12AL08G]en
dc.language.isoenen
dc.publisherAMER GEOPHYSICAL UNIONen
dc.relation.urlhttp://doi.wiley.com/10.1002/2016JE005090en
dc.rights©2016. American Geophysical Union. All Rights Reserved.en
dc.titleInteractions between complex craters and the lunar crust: Analysis using GRAIL dataen
dc.typeArticleen
dc.contributor.departmentUniv Arizona, Lunar & Planetary Laben
dc.identifier.journalJournal of Geophysical Research: Planetsen
dc.description.noteFirst Published: 25 August 2016; 6 Month Embargo.en
dc.description.collectioninformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.en
dc.eprint.versionFinal published versionen
dc.contributor.institutionDepartment of Earth and Planetary Sciences; University of California; Santa Cruz California USA
dc.contributor.institutionPlanetary Science Directorate; Southwest Research Institute; Boulder Colorado USA
dc.contributor.institutionDepartment of Earth and Planetary Sciences; University of California; Santa Cruz California USA
dc.contributor.institutionEnseignant Indépendant (SIREN 819716788); Nantes France
dc.contributor.institutionDepartment of Earth, Atmospheric, and Planetary Sciences; Purdue University; West Lafayette Indiana USA
dc.contributor.institutionLunar and Planetary Laboratory; University of Arizona; Tucson Arizona USA
dc.contributor.institutionDepartment of Earth, Atmospheric and Planetary Sciences; Massachusetts Institute of Technology; Cambridge Massachusetts USA
dc.contributor.institutionDepartment of Earth, Atmospheric and Planetary Sciences; Massachusetts Institute of Technology; Cambridge Massachusetts USA
refterms.dateFOA2017-08-26T00:00:00Z
html.description.abstractA high-resolution gravity map over the entire lunar surface has been derived from data acquired by the Gravity Recovery and Interior Laboratory (GRAIL) mission. Soderblom et al. (2015) showed that crater Bouguer gravity anomalies scale with crater diameter and porosity for craters in the lunar highlands. Here we extend this study globally, examining complex craters in each of the three lunar terranes: highlands, maria, and the South Pole-Aitken basin. We find that craters within South Pole-Aitken basin and in the lunar maria have statistically different Bouguer anomalies from those in the lunar highlands. These differences are best explained by differences in crustal porosity among the three terranes. Though there is still much unresolved scatter in the data, we find that no other lunar material properties (crustal thickness, density gradient, etc.) are able to improve our model fit to the data.


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