View in EDS

Impact cratering experiments in brittle targets with variable thickness: Implications for deep pit craters on Mars.

Saved in:
Bibliographic Details
Title: Impact cratering experiments in brittle targets with variable thickness: Implications for deep pit craters on Mars.
Authors: Michikami, T.1 michikami@hiro.kindai.ac.jp, Hagermann, A.2, Miyamoto, H.3, Miura, S.4, Haruyama, J.5, Lykawka, P.S.6
Source: Planetary & Space Science. Jun2014, Vol. 96, p71-80. 10p.
Subjects: Martian craters, Compressive strength, Nylon, Martian surface, Observations of Mars
Abstract: Abstract: High-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 1–6cm, and a bulk density of 1550kg/m3 by using a mixture of cement, water and sand (0.2mm) in the ratio of 1:1:10, by weight. The compressive strength of the resulting targets is 3.2±0.9MPa. A spherical nylon projectile (diameter 7mm) is shot perpendicularly into the target surface at the nominal velocity of 1.2km/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. [Copyright &y& Elsevier]
Copyright of Planetary & Space Science is the property of Pergamon Press - An Imprint of Elsevier Science and its content may not be copied or emailed to multiple sites without the copyright holder's express written permission. Additionally, content may not be used with any artificial intelligence tools or machine learning technologies. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract. (Copyright applies to all Abstracts.)
Database: Engineering Source
FullText Text:
  Availability: 0
Header DbId: egs
DbLabel: Engineering Source
An: 96188168
AccessLevel: 6
PubType: Academic Journal
PubTypeId: academicJournal
PreciseRelevancyScore: 0
IllustrationInfo
Items – Name: Title
  Label: Title
  Group: Ti
  Data: Impact cratering experiments in brittle targets with variable thickness: Implications for deep pit craters on Mars.
– Name: Author
  Label: Authors
  Group: Au
  Data: <searchLink fieldCode="AR" term="%22Michikami%2C+T%2E%22">Michikami, T.</searchLink><relatesTo>1</relatesTo><i> michikami@hiro.kindai.ac.jp</i><br /><searchLink fieldCode="AR" term="%22Hagermann%2C+A%2E%22">Hagermann, A.</searchLink><relatesTo>2</relatesTo><br /><searchLink fieldCode="AR" term="%22Miyamoto%2C+H%2E%22">Miyamoto, H.</searchLink><relatesTo>3</relatesTo><br /><searchLink fieldCode="AR" term="%22Miura%2C+S%2E%22">Miura, S.</searchLink><relatesTo>4</relatesTo><br /><searchLink fieldCode="AR" term="%22Haruyama%2C+J%2E%22">Haruyama, J.</searchLink><relatesTo>5</relatesTo><br /><searchLink fieldCode="AR" term="%22Lykawka%2C+P%2ES%2E%22">Lykawka, P.S.</searchLink><relatesTo>6</relatesTo>
– Name: TitleSource
  Label: Source
  Group: Src
  Data: <searchLink fieldCode="JN" term="%22Planetary+%26+Space+Science%22">Planetary & Space Science</searchLink>. Jun2014, Vol. 96, p71-80. 10p.
– Name: Subject
  Label: Subjects
  Group: Su
  Data: <searchLink fieldCode="DE" term="%22Martian+craters%22">Martian craters</searchLink><br /><searchLink fieldCode="DE" term="%22Compressive+strength%22">Compressive strength</searchLink><br /><searchLink fieldCode="DE" term="%22Nylon%22">Nylon</searchLink><br /><searchLink fieldCode="DE" term="%22Martian+surface%22">Martian surface</searchLink><br /><searchLink fieldCode="DE" term="%22Observations+of+Mars%22">Observations of Mars</searchLink>
– Name: Abstract
  Label: Abstract
  Group: Ab
  Data: Abstract: High-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 1–6cm, and a bulk density of 1550kg/m3 by using a mixture of cement, water and sand (0.2mm) in the ratio of 1:1:10, by weight. The compressive strength of the resulting targets is 3.2±0.9MPa. A spherical nylon projectile (diameter 7mm) is shot perpendicularly into the target surface at the nominal velocity of 1.2km/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. [Copyright &y& Elsevier]
– Name: AbstractSuppliedCopyright
  Label:
  Group: Ab
  Data: <i>Copyright of Planetary & Space Science is the property of Pergamon Press - An Imprint of Elsevier Science and its content may not be copied or emailed to multiple sites without the copyright holder's express written permission. Additionally, content may not be used with any artificial intelligence tools or machine learning technologies. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract.</i> (Copyright applies to all Abstracts.)
PLink https://search.ebscohost.com/login.aspx?direct=true&site=eds-live&db=egs&AN=96188168
RecordInfo BibRecord:
  BibEntity:
    Identifiers:
      – Type: doi
        Value: 10.1016/j.pss.2014.03.010
    Languages:
      – Code: eng
        Text: English
    PhysicalDescription:
      Pagination:
        PageCount: 10
        StartPage: 71
    Subjects:
      – SubjectFull: Martian craters
        Type: general
      – SubjectFull: Compressive strength
        Type: general
      – SubjectFull: Nylon
        Type: general
      – SubjectFull: Martian surface
        Type: general
      – SubjectFull: Observations of Mars
        Type: general
    Titles:
      – TitleFull: Impact cratering experiments in brittle targets with variable thickness: Implications for deep pit craters on Mars.
        Type: main
  BibRelationships:
    HasContributorRelationships:
      – PersonEntity:
          Name:
            NameFull: Michikami, T.
      – PersonEntity:
          Name:
            NameFull: Hagermann, A.
      – PersonEntity:
          Name:
            NameFull: Miyamoto, H.
      – PersonEntity:
          Name:
            NameFull: Miura, S.
      – PersonEntity:
          Name:
            NameFull: Haruyama, J.
      – PersonEntity:
          Name:
            NameFull: Lykawka, P.S.
    IsPartOfRelationships:
      – BibEntity:
          Dates:
            – D: 01
              M: 06
              Text: Jun2014
              Type: published
              Y: 2014
          Identifiers:
            – Type: issn-print
              Value: 00320633
          Numbering:
            – Type: volume
              Value: 96
          Titles:
            – TitleFull: Planetary & Space Science
              Type: main
ResultId 1