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dc.contributor.authorHorton, J. Wright
dc.contributor.authorOrmö, Jens
dc.contributor.authorPowars, David S.
dc.contributor.authorGohn, Gregory S.
dc.date.accessioned2021-02-12T21:41:01Z
dc.date.available2021-02-12T21:41:01Z
dc.date.issued2006-01-01
dc.identifier.citationHorton, J. W., Ormö, J., Powars, D. S., & Gohn, G. S. (2006). Chesapeake Bay impact structure: Morphology, crater fill, and relevance for impact structures on Mars. Meteoritics & Planetary Science, 41(10), 1613-1624.
dc.identifier.issn1945-5100
dc.identifier.doi10.1111/j.1945-5100.2006.tb00439.x
dc.identifier.urihttp://hdl.handle.net/10150/656202
dc.descriptionFrom the proceedings of the Workshop on the Role of Volatiles and Atmospheres on Martian Impact Craters held on July 11-14, 2005, at the Johns Hopkins University Applied Physics Laboratory.
dc.description.abstractThe late Eocene Chesapeake Bay impact structure (CBIS) on the Atlantic margin of Virginia is one of the largest and best-preserved "wet-target" craters on Earth. It provides an accessible analog for studying impact processes in layered and wet targets on volatile-rich planets. The CBIS formed in a layered target of water, weak clastic sediments, and hard crystalline rock. The buried structure consists of a deep, filled central crater, 38 km in width, surrounded by a shallower brim known as the annular trough. The annular trough formed partly by collapse of weak sediments, which expanded the structure to ~85 km in diameter. Such extensive collapse, in addition to excavation processes, can explain the "inverted sombrero" morphology observed at some craters in layered targets.The distribution of crater-fill materials in the CBIS is related to the morphology. Suevitic breccia, including pre-resurge fallback deposits, is found in the central crater. Impact-modified sediments, formed by fluidization and collapse of water-saturated sand and silt-clay, occur in the annular trough. Allogenic sediment-clast breccia, interpreted as ocean-resurge deposits, overlies the other impactites and covers the entire crater beneath a blanket of postimpact sediments.The formation of chaotic terrains on Mars is attributed to collapse due to the release of volatiles from thick layered deposits. Some flat-floored rimless depressions with chaotic infill in these terrains are impact craters that expanded by collapse farther than expected for similar-sized complex craters in solid targets. Studies of crater materials in the CBIS provide insights into processes of crater expansion on Mars and their links to volatiles.
dc.language.isoen
dc.publisherThe Meteoritical Society
dc.relation.urlhttps://meteoritical.org/
dc.rightsCopyright © The Meteoritical Society
dc.rights.urihttp://rightsstatements.org/vocab/InC/1.0/
dc.subjectPlanet Mars
dc.subjectimpact craters
dc.subjectChesapeake Bay
dc.subjectVirginia
dc.subjectimpact breccias
dc.subjectimpact crater USA
dc.titleChesapeake Bay impact structure: Morphology, crater fill, and relevance for impact structures on Mars
dc.typeProceedings
dc.typetext
dc.identifier.journalMeteoritics & Planetary Science
dc.description.collectioninformationThe Meteoritics & Planetary Science archives are made available by the Meteoritical Society and the University of Arizona Libraries. Contact lbry-journals@email.arizona.edu for further information.
dc.eprint.versionFinal published version
dc.description.admin-noteMigrated from OJS platform February 2021
dc.source.volume41
dc.source.issue10
dc.source.beginpage1613
dc.source.endpage1624
refterms.dateFOA2021-02-12T21:41:01Z


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