43rd Lunar and Planetary Science Conference (2012) 2388.pdf NEW LUNAR IMPACT MELT FLOWS AS REVEALED BY MINI-RF ON LRO. C. D. Neish1, N. Glines2, L. M. Carter3, V. J. Bray4, B. R. Hawke5, D. B. J. Bussey1, and the Mini-RF Science Team, 1The Johns Hopkins University Applied Physics Laboratory, Laurel, MD, 20723 (
[email protected]), 2Mount Holyoke College, South Hadley, MA, 01075, 3NASA Goddard Spaceflight Center, Greenbelt, MD, 20770, 4The University of Ari- zona, Tucson, AZ, 85721, 5The University of Hawai’i at Manoa, Honolulu, HI, 96822. Introduction: Flow-like deposits of impact melt fying impact melts. After a candidate melt is identified, are commonly observed on the Moon, typically around data from the LRO Camera (LROC) was used to iden- young fresh craters. These flows are thought to be mix- tify additional features associated with impact melt tures of clasts and melted material that are emplaced deposits, such as cooling cracks in ponds and tension during the late stages of impact crater formation [1]. cracks in veneers, confirming these features as impact Lunar impact melts have been primarily studied at op- melts. tical wavelengths, but complementary information can be obtained by observing impact melts at radar wave- lengths. Radar data is sensitive to surface and sub- surface roughness, and thus can highlight these rough surface features, even when they not easily seen in optical data due to burial or imperfect lighting condi- tions (Fig. 1). Impact melts have been identified in radar data on the lunar near side [2], but they have yet to be studied in depth on the lunar far side, given the lack of global radar data prior to the launch of NASA’s Mini-RF instrument on the Lunar Reconnaissance Or- biter (LRO) in 2009.