Initial observations of lunar impact melts and ejecta flows with the Mini-RF radar

Details Initial observations of lunar impact melts and ejecta flows with the Mini-RF radar Initial observations of lunar impact melts and ejecta flows with the Mini-RF radar

Feb 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012jgre..11700h09c&link_type=abstract

Journal of Geophysical Research, Volume 117, CiteID E00H09

Astronomy and Astrophysics

Astronomy

1

Planetary Sciences: Solid Surface Planets: Impact Phenomena, Cratering (6022, 8136), Planetary Sciences: Solid Surface Planets: Surface Materials And Properties, Planetary Sciences: Solar System Objects: Moon (1221), Radio Science: Radio Astronomy, Radio Science: Remote Sensing

Scientific paper

The Mini-RF radar on the Lunar Reconnaissance Orbiter spacecraft has revealed a great variety of crater ejecta flow and impact melt deposits, some of which were not observed in prior radar imaging. The craters Tycho and Glushko have long melt flows that exhibit variations in radar backscatter and circular polarization ratio along the flow. Comparison with optical imaging reveals that these changes are caused by features commonly seen in terrestrial lava flows, such as rafted plates, pressure ridges, and ponding. Small (<20 km) sized craters also show a large variety of deposits, including melt flows and ponds. Two craters have flow features that may be ejecta flows caused by entrained debris flowing across the surface rather than by melted rock. The circular polarization ratios (CPRs) of the impact melt flows are typically very high; even ponded areas have CPR values between 0.7 and 1.0. This high CPR suggests that deposits that appear smooth in optical imagery may be rough at centimeter- and decimeter- scales. In some places, ponds and flows are visible with no easily discernable source crater. These melt deposits may have come from oblique impacts that are capable of ejecting melted material farther downrange. They may also be associated with older, nearby craters that no longer have a radar-bright proximal ejecta blanket. The observed morphology of the lunar crater flows has implications for similar features observed on Venus. In particular, changes in backscatter along many of the ejecta flows are probably caused by features typical of lava flows.

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