Orbital infrared observations of lunar craters and possible implications for impact ejecta emplacement

dc.contributor.author	Schultz, Peter H., 1944-
dc.contributor.author	Mendell, W. W. (Wendell W.), 1941-
dc.coverage.spatial	Moon
dc.date.accessioned	2020-05-18T20:27:15Z
dc.date.available	2020-05-18T20:27:15Z
dc.date.issued	1978
dc.description.abstract	The Apollo 17 Scanning Infrared Radiometer experiment showed that the ejecta deposits of large lunar craters (D greater than 3 km) typically exhibit uniform nighttime temperatures comparable to or less than those of the surrounding mare plains. This thermal signature implies that the surface of ejecta deposits displays block sizes typically smaller than 30 cm and that the nonblocky surface extends out to three crater radii from the crater rim. Four mechanisms are proposed to account for the observed thermal signatures.	en
dc.description.statementofresponsibility	Peter H. Schultz, Lunar and Planetary Institute, 3303 NASA Road 1, Houston, Texas 77058, Wendell Mendell, NASA-Johnson Space Center, Houston, Texas 77058
dc.format.extent	Pages 2857-2883
dc.format.mimetype	application/pdf
dc.identifier.uri	https://hdl.handle.net/20.500.11753/1532
dc.language.iso	en	en
dc.publisher	Pergamon Press	en
dc.relation.ispartof	Proceedings of the Ninth Lunar and Planetary Science Conference
dc.relation.ispartofseries	LPI contribution ; no. 342
dc.subject	Moon--Temperature and radiation	en
dc.subject	Lunar craters	en
dc.title	Orbital infrared observations of lunar craters and possible implications for impact ejecta emplacement	en
dc.type	Book chapter	en

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