Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufm.p31b1409t&link_type=abstract
American Geophysical Union, Fall Meeting 2008, abstract #P31B-1409
Astronomy and Astrophysics
Astronomy
1160 Planetary And Lunar Geochronology, 5420 Impact Phenomena, Cratering (6022, 8136), 5464 Remote Sensing, 6949 Radar Astronomy, 6969 Remote Sensing
Scientific paper
The southern highlands of the Moon comprise superposed ejecta layers, individually up to a kilometer in thickness, from the major basins. The radar properties of smaller (1-16 km diameter) impact craters that penetrate into this layered mega-regolith and excavate material from depth provide insight into the variability of mega-regolith depth above a postulated basement of large crustal blocks. We observe a significant difference in the population of radar-bright craters, 1-16 km and larger in diameter, between regions of the southeastern nearside highlands north and south of approximately 48°S latitude. There are about 1/3 fewer radar-bright craters south of this line than to the north, broadly coincident with the mapped boundary between southern deposits mapped as pre-Nectarian age and those of Nectarian to Imbrian age to the north. This difference in small radar-bright crater population is consistent with a mega-regolith thickness of about 1.5 km in the north and 2.5 km in the south, a difference that we attribute to South-Pole-Aitken basin ejecta.
Campbell Bruce A.
Ghent Rebecca R.
Hawke B. B.
Thompson William T.
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