Physical constraints on impact melt properties from Lunar Reconnaissance Orbiter Camera images

Brett W. Denevi; Steven D. Koeber; Mark Robinson; W. Brent Garry; B. Ray Hawke; Thanh N. Tran; Samuel J. Lawrence; Laszlo P. Keszthelyi; Olivier S. Barnouin; Carolyn M. Ernst; Livio L. Tornabene

doi:10.1016/j.icarus.2012.03.020

Physical constraints on impact melt properties from Lunar Reconnaissance Orbiter Camera images

Brett W. Denevi, Steven D. Koeber, Mark Robinson, W. Brent Garry, B. Ray Hawke, Thanh N. Tran, Samuel J. Lawrence, Laszlo P. Keszthelyi, Olivier S. Barnouin, Carolyn M. Ernst, Livio L. Tornabene

Earth and Space Exploration, School of (SESE)

Research output: Contribution to journal › Article › peer-review

47 Scopus citations

Abstract

Impact melt flows exterior to Copernican-age craters are observed in high spatial resolution (0.5. m/pixel) images acquired by the Lunar Reconnaissance Orbiter Camera (LROC) Narrow Angle Camera (NAC). Impact melt is mapped in detail around 15 craters ranging in diameter from 2.4 to 32.5. km. This survey supports previous observations suggesting melt flows often occur at craters whose shape is influenced by topographic variation at the pre-impact site. Impact melt flows are observed around craters as small as 2.4. km in diameter, and preliminary estimates of melt volume suggest melt production at small craters can significantly exceed model predictions. Digital terrain models produced from targeted NAC stereo images are used to examine the three-dimensional properties of flow features and emplacement setting, enabling physical modeling of flow parameters. Qualitative and quantitative observations are consistent with low-viscosity melts heated above their liquidii (superheated) with limited amounts of entrained solids.

Original language	English (US)
Pages (from-to)	665-675
Number of pages	11
Journal	Icarus
Volume	219
Issue number	2
DOIs	https://doi.org/10.1016/j.icarus.2012.03.020
State	Published - Jun 2012

Keywords

Cratering
Moon
Moon, Surface

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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10.1016/j.icarus.2012.03.020

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title = "Physical constraints on impact melt properties from Lunar Reconnaissance Orbiter Camera images",

abstract = "Impact melt flows exterior to Copernican-age craters are observed in high spatial resolution (0.5. m/pixel) images acquired by the Lunar Reconnaissance Orbiter Camera (LROC) Narrow Angle Camera (NAC). Impact melt is mapped in detail around 15 craters ranging in diameter from 2.4 to 32.5. km. This survey supports previous observations suggesting melt flows often occur at craters whose shape is influenced by topographic variation at the pre-impact site. Impact melt flows are observed around craters as small as 2.4. km in diameter, and preliminary estimates of melt volume suggest melt production at small craters can significantly exceed model predictions. Digital terrain models produced from targeted NAC stereo images are used to examine the three-dimensional properties of flow features and emplacement setting, enabling physical modeling of flow parameters. Qualitative and quantitative observations are consistent with low-viscosity melts heated above their liquidii (superheated) with limited amounts of entrained solids.",

keywords = "Cratering, Moon, Moon, Surface",

author = "Denevi, {Brett W.} and Koeber, {Steven D.} and Mark Robinson and Garry, {W. Brent} and Hawke, {B. Ray} and Tran, {Thanh N.} and Lawrence, {Samuel J.} and Keszthelyi, {Laszlo P.} and Barnouin, {Olivier S.} and Ernst, {Carolyn M.} and Tornabene, {Livio L.}",

note = "Funding Information: We gratefully acknowledge the LRO and LROC engineers and operations personnel. We thank Mike Malin for insightful input, and reviewers Scott Rowland and Veronica Bray for constructive and thoughtful reviews. This work was supported by the National Aeronautics and Space Administration Lunar Reconnaissance Orbiter Project.",

year = "2012",

month = jun,

doi = "10.1016/j.icarus.2012.03.020",

language = "English (US)",

volume = "219",

pages = "665--675",

journal = "Icarus",

issn = "0019-1035",

publisher = "Academic Press Inc.",

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AU - Denevi, Brett W.

AU - Koeber, Steven D.

AU - Robinson, Mark

AU - Garry, W. Brent

AU - Hawke, B. Ray

AU - Tran, Thanh N.

AU - Lawrence, Samuel J.

AU - Keszthelyi, Laszlo P.

AU - Barnouin, Olivier S.

AU - Ernst, Carolyn M.

AU - Tornabene, Livio L.

N1 - Funding Information: We gratefully acknowledge the LRO and LROC engineers and operations personnel. We thank Mike Malin for insightful input, and reviewers Scott Rowland and Veronica Bray for constructive and thoughtful reviews. This work was supported by the National Aeronautics and Space Administration Lunar Reconnaissance Orbiter Project.

PY - 2012/6

Y1 - 2012/6

N2 - Impact melt flows exterior to Copernican-age craters are observed in high spatial resolution (0.5. m/pixel) images acquired by the Lunar Reconnaissance Orbiter Camera (LROC) Narrow Angle Camera (NAC). Impact melt is mapped in detail around 15 craters ranging in diameter from 2.4 to 32.5. km. This survey supports previous observations suggesting melt flows often occur at craters whose shape is influenced by topographic variation at the pre-impact site. Impact melt flows are observed around craters as small as 2.4. km in diameter, and preliminary estimates of melt volume suggest melt production at small craters can significantly exceed model predictions. Digital terrain models produced from targeted NAC stereo images are used to examine the three-dimensional properties of flow features and emplacement setting, enabling physical modeling of flow parameters. Qualitative and quantitative observations are consistent with low-viscosity melts heated above their liquidii (superheated) with limited amounts of entrained solids.

AB - Impact melt flows exterior to Copernican-age craters are observed in high spatial resolution (0.5. m/pixel) images acquired by the Lunar Reconnaissance Orbiter Camera (LROC) Narrow Angle Camera (NAC). Impact melt is mapped in detail around 15 craters ranging in diameter from 2.4 to 32.5. km. This survey supports previous observations suggesting melt flows often occur at craters whose shape is influenced by topographic variation at the pre-impact site. Impact melt flows are observed around craters as small as 2.4. km in diameter, and preliminary estimates of melt volume suggest melt production at small craters can significantly exceed model predictions. Digital terrain models produced from targeted NAC stereo images are used to examine the three-dimensional properties of flow features and emplacement setting, enabling physical modeling of flow parameters. Qualitative and quantitative observations are consistent with low-viscosity melts heated above their liquidii (superheated) with limited amounts of entrained solids.

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KW - Moon, Surface

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Physical constraints on impact melt properties from Lunar Reconnaissance Orbiter Camera images

Abstract

Keywords

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