Surface waves and crustal structure on Mars

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dc.contributor.authorKim, D.en
dc.contributor.authorBanerdt, W. B.en
dc.contributor.authorCeylan, S.en
dc.contributor.authorGiardini, D.en
dc.contributor.authorLekic, V.en
dc.contributor.authorLognonne, P.en
dc.contributor.authorBeghein, C.en
dc.contributor.authorBeucler, E.en
dc.contributor.authorCarrasco, S.en
dc.contributor.authorCharalambous, C.en
dc.contributor.authorClinton, J.en
dc.contributor.authorDrilleau, M.en
dc.contributor.authorDuran, C.en
dc.contributor.authorGolombek, M.en
dc.contributor.authorJoshi, R.en
dc.contributor.authorKhan, A.en
dc.contributor.authorKnapmeyer-Endrun, B.en
dc.contributor.authorLi, J.en
dc.contributor.authorMaguire, R.en
dc.contributor.authorPike, W. T.en
dc.contributor.authorSamuel, H.en
dc.contributor.authorSchimmel, M.en
dc.contributor.authorSchmerr, N. C.en
dc.contributor.authorStahler, S. C.en
dc.contributor.authorStutzmann, E.en
dc.contributor.authorWieczorek, M.en
dc.contributor.authorXu, Z.en
dc.contributor.authorBatov, A.en
dc.contributor.authorBozdag, E.en
dc.contributor.authorDahmen, N.en
dc.contributor.authorDavis, P.en
dc.contributor.authorGudkova, T.en
dc.contributor.authorHorleston, A.en
dc.contributor.authorHuang, Q.en
dc.contributor.authorKawamura, T.en
dc.contributor.authorKing, Scott D.en
dc.contributor.authorMcLennan, S. M.en
dc.contributor.authorNimmo, F.en
dc.contributor.authorPlasman, M.en
dc.contributor.authorPlesa, A. C.en
dc.contributor.authorStepanova, I. E.en
dc.contributor.authorWeidner, E.en
dc.contributor.authorZenhausern, G.en
dc.contributor.authorDaubar, I. J.en
dc.contributor.authorFernando, B.en
dc.contributor.authorGarcia, R. F.en
dc.contributor.authorPosiolova, L.en
dc.contributor.authorPanning, M. P.en
dc.date.accessioned2024-01-17T17:25:56Zen
dc.date.available2024-01-17T17:25:56Zen
dc.date.issued2022-10-28en
dc.description.abstractWe detected surface waves from two meteorite impacts on Mars. By measuring group velocity dispersion along the impact-lander path, we obtained a direct constraint on crustal structure away from the InSight lander. The crust north of the equatorial dichotomy had a shear wave velocity of approximately 3.2 kilometers per second in the 5- to 30-kilometer depth range, with little depth variation. This implies a higher crustal density than inferred beneath the lander, suggesting either compositional differences or reduced porosity in the volcanic areas traversed by the surface waves. The lower velocities and the crustal layering observed beneath the landing site down to a 10-kilometer depth are not a global feature. Structural variations revealed by surface waves hold implications for models of the formation and thickness of the martian crust.en
dc.description.versionAccepted versionen
dc.format.extentPages 417-421en
dc.format.extent5 page(s)en
dc.identifier.doihttps://doi.org/10.1126/science.abq7157en
dc.identifier.eissn1095-9203en
dc.identifier.issn0036-8075en
dc.identifier.issue6618en
dc.identifier.orcidKing, Scott [0000-0002-9564-5164]en
dc.identifier.pmid36302020en
dc.identifier.urihttps://hdl.handle.net/10919/117381en
dc.identifier.volume378en
dc.publisherAAASen
dc.relation.urihttps://www.ncbi.nlm.nih.gov/pubmed/36302020en
dc.rightsIn Copyrighten
dc.rights.urihttp://rightsstatements.org/vocab/InC/1.0/en
dc.subjectMarsen
dc.subjectInSighten
dc.subjectCrusten
dc.titleSurface waves and crustal structure on Marsen
dc.title.serialScienceen
dc.typeArticle - Refereeden
dc.type.otherArticleen
dc.type.otherJournalen
pubs.organisational-group/Virginia Techen
pubs.organisational-group/Virginia Tech/Scienceen
pubs.organisational-group/Virginia Tech/Science/Geosciencesen
pubs.organisational-group/Virginia Tech/All T&R Facultyen
pubs.organisational-group/Virginia Tech/Science/COS T&R Facultyen

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