Non-basaltic early lunar magmatism

Details Non-basaltic early lunar magmatism Non-basaltic early lunar magmatism

Mar 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997lpi....28.1577w&link_type=abstract

Conference Paper, 28th Annual Lunar and Planetary Science Conference, p. 577.

Other

Lunar Craters, Magma, Hypervelocity Impact, Meteorite Craters, Lunar Crust, Volcanoes, Anorthosite, Cratering, Lunar Maria, Planetary Geology

Scientific paper

The early history of the moon was dominated by impact cratering and volcanic resurfacing. By 4.5 billion years ago, the moon had accreted by impact cratering that was a billion times more intense than today. The energy of accretion provided enough heat to totally melt the moon, or at least the top few hundred kilometers, causing the formation of the global anorthositic crust. Both cratering and magmatism declined, apparently at differing rates. By 3.8 billion years ago, cratering was reduced to rates only a few times higher than today, but mare volcanism was still intense for another 300 to 800 million years. As we look at the moon today we can generally recognize and understand the volcanic and impact units since 4.0 billion years ago, but identification of the origins of earlier deposits are still controversial. I propose that mare volcanism was simply the last, and most distinct in the albedo phase of widespread early lunar magmatism. The only places that preserve the earlier volcanism are the lunar highlands.

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