Rugged lava flows on the Moon revealed by Earth-based radar

Details Rugged lava flows on the Moon revealed by Earth-based radar Rugged lava flows on the Moon revealed by Earth-based radar

Nov 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009georl..3622201c&link_type=abstract

Geophysical Research Letters, Volume 36, Issue 22, CiteID L22201

Physics

6

Planetary Sciences: Solid Surface Planets: Volcanism (6063, 8148, 8450), Planetary Sciences: Solid Surface Planets: Remote Sensing, Planetary Sciences: Solid Surface Planets: Surface Materials And Properties

Scientific paper

Basaltic volcanism is widespread on the lunar nearside, and returned samples suggest that the mare-forming magmas had low viscosity that led to primarily sheet-like deposits. New 70-cm wavelength radar observations that probe several meters beneath the lunar surface reveal differences in mare backscatter properties not explained by age or compositional variations. We interpret areas of high backscatter and high circular polarization ratio in Maria Serenitatis, Imbrium, and Crisium as having an enhanced abundance of decimeter-scale subsurface rocks relative to typical mare-forming flows. The 3.5 b.y survival of these differences implies an initial platy, blocky, or ridged lava flow surface layer with thickness of at least 3-5 m. Such rugged morphology might arise from episodic changes in magma effusion rate, as observed for disrupted flood basalt surfaces on the Earth and Mars, very high flow velocities, or increased viscosity due to a number of factors. Significant information on lunar mare eruption conditions may thus be obtained from long-wavelength radar probing of the shallow subsurface.

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