Please use this identifier to cite or link to this item: http://hdl.handle.net/1893/27540
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dc.contributor.authorMichikami, Tatsuhiroen_UK
dc.contributor.authorHagermann, Axelen_UK
dc.contributor.authorMiyamoto, Hideakien_UK
dc.contributor.authorMiura, Seiichien_UK
dc.contributor.authorHaruyama, Junichien_UK
dc.contributor.authorLykawka, Patryk Sen_UK
dc.date.accessioned2018-07-24T00:04:55Z-
dc.date.available2018-07-24T00:04:55Z-
dc.date.issued2014-06-30en_UK
dc.identifier.urihttp://hdl.handle.net/1893/27540-
dc.description.abstractHigh-resolution images reveal that numerous pit craters exist on the surface of Mars. For some pit craters, the depth-to-diameter ratios are much greater than for ordinary craters. Such deep pit craters are generally considered to be the results of material drainage into a subsurface void space, which might be formed by a lava tube, dike injection, extensional fracturing, and dilational normal faulting. Morphological studies indicate that the formation of a pit crater might be triggered by the impact event, and followed by collapse of the ceiling. To test this hypothesis, we carried out laboratory experiments of impact cratering into brittle targets with variable roof thickness. In particular, the effect of the target thickness on the crater formation is studied to understand the penetration process by an impact. For this purpose, we produced mortar targets with roof thickness of 1-6 cm, and a bulk density of 1550 kg/m3 by using a mixture of cement, water and sand (0.2 mm) in the ratio of 1:1:10, by weight. The compressive strength of the resulting targets is 3.2±0.9 MPa. A spherical nylon projectile (diameter 7 mm) is shot perpendicularly into the target surface at the nominal velocity of 1.2 km/s, using a two-stage light-gas gun. Craters are formed on the opposite side of the impact even when no target penetration occurs. Penetration of the target is achieved when craters on the opposite sides of the target connect with each other. In this case, the cross section of crater somehow attains a flat hourglass-like shape. We also find that the crater diameter on the opposite side is larger than that on the impact side, and more fragments are ejected from the crater on the opposite side than from the crater on the impact side. This result gives a qualitative explanation for the observation that the Martian deep pit craters lack a raised rim and have the ejecta deposit on their floor instead. © 2014 Elsevier Ltd. All rights reserved.en_UK
dc.language.isoenen_UK
dc.publisherElsevieren_UK
dc.relationMichikami T, Hagermann A, Miyamoto H, Miura S, Haruyama J & Lykawka PS (2014) Impact cratering experiments in brittle targets with variable thickness: Implications for deep pit craters on Mars. Planetary and Space Science, 96, pp. 71-80. https://doi.org/10.1016/j.pss.2014.03.010en_UK
dc.rightsThis article is available under the terms of the Creative Commons Attribution License (CC BY). You may distribute and copy the article, create extracts, abstracts, and other revised versions, adaptations or derivative works of or from an article (such as a translation), to include in a collective work (such as an anthology), to text or data mine the article, including for commercial purposes without permission from Elsevier. The original work must always be appropriately credited.en_UK
dc.rights.urihttp://creativecommons.org/licenses/by/3.0/en_UK
dc.subjectImpact cratering processen_UK
dc.subjectpit crateren_UK
dc.subjectpenetration regimeen_UK
dc.subjectsubsurface cavityen_UK
dc.subjectlaboratory experimentsen_UK
dc.titleImpact cratering experiments in brittle targets with variable thickness: Implications for deep pit craters on Marsen_UK
dc.typeJournal Articleen_UK
dc.identifier.doi10.1016/j.pss.2014.03.010en_UK
dc.citation.jtitlePlanetary and Space Scienceen_UK
dc.citation.issn0032-0633en_UK
dc.citation.volume96en_UK
dc.citation.spage71en_UK
dc.citation.epage80en_UK
dc.citation.publicationstatusPublisheden_UK
dc.citation.peerreviewedRefereeden_UK
dc.type.statusVoR - Version of Recorden_UK
dc.contributor.funderScience & Technology Facilities Councilen_UK
dc.citation.date25/03/2014en_UK
dc.contributor.affiliationKindai Universityen_UK
dc.contributor.affiliationThe Open Universityen_UK
dc.contributor.affiliationUniversity of Tokyoen_UK
dc.contributor.affiliationTokuyama College of Technologyen_UK
dc.contributor.affiliationJapan Aerospace Exploration Agencyen_UK
dc.contributor.affiliationKindai Universityen_UK
dc.identifier.isiWOS:000336824600007en_UK
dc.identifier.scopusid2-s2.0-84901375807en_UK
dc.identifier.wtid493351en_UK
dc.contributor.orcid0000-0002-1818-9396en_UK
dc.date.accepted2014-03-12en_UK
dcterms.dateAccepted2014-03-12en_UK
dc.date.filedepositdate2018-07-05en_UK
rioxxterms.apcnot requireden_UK
rioxxterms.typeJournal Article/Reviewen_UK
rioxxterms.versionVoRen_UK
local.rioxx.authorMichikami, Tatsuhiro|en_UK
local.rioxx.authorHagermann, Axel|0000-0002-1818-9396en_UK
local.rioxx.authorMiyamoto, Hideaki|en_UK
local.rioxx.authorMiura, Seiichi|en_UK
local.rioxx.authorHaruyama, Junichi|en_UK
local.rioxx.authorLykawka, Patryk S|en_UK
local.rioxx.projectProject ID unknown|Science & Technology Facilities Council|en_UK
local.rioxx.freetoreaddate2018-07-05en_UK
local.rioxx.licencehttp://creativecommons.org/licenses/by/3.0/|2018-07-05|en_UK
local.rioxx.filenameMichikami et al 2014.pdfen_UK
local.rioxx.filecount1en_UK
local.rioxx.source0032-0633en_UK
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