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Small rayed crater ejecta retention age calculated from current crater production rates on Mars

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dc.contributor.author Calef, F. J. III
dc.contributor.author Herrick, R. R.
dc.contributor.author Sharpton, V. L.
dc.date.accessioned 2013-08-07T21:35:58Z
dc.date.available 2013-08-07T21:35:58Z
dc.date.issued 2011-03-03
dc.identifier.citation 42 Lunar and Planetary Institute Conference, Woodlands, Texas, March 7–11, 2011 en_US
dc.identifier.clearanceno 11-0841
dc.identifier.uri http://hdl.handle.net/2014/43474
dc.description.abstract Ejecta from impact craters, while extant, records erosive and depositional processes on their surfaces. Estimating ejecta retention age (Eret), the time span when ejecta remains recognizable around a crater, can be applied to estimate the timescale that surface processes operate on, thereby obtaining a history of geologic activity. However, the abundance of sub-kilometer diameter (D) craters identifiable in highresolution Mars imagery has led to questions of accuracy in absolute crater dating and hence ejecta retention ages (Eret). This research calculates the maximum Eret for small rayed impact craters (SRC) on Mars using estimates of the Martian impactor flux adjusted for meteorite ablation losses in the atmosphere. In addition, we utilize the diameter-distance relationship of secondary cratering to adjust crater counts in the vicinity of the large primary crater Zunil. en_US
dc.description.sponsorship NASA/JPL en_US
dc.language.iso en_US en_US
dc.publisher Pasadena, CA : Jet Propulsion Laboratory, National Aeronautics and Space Administration, 2011. en_US
dc.subject Mars en_US
dc.subject Rayed Craters en_US
dc.subject Ejecta Retention Rate en_US
dc.title Small rayed crater ejecta retention age calculated from current crater production rates on Mars en_US
dc.type Preprint en_US


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