Ages, Thicknesses and Mineralogy of Lunar Mare Basalts

Details Ages, Thicknesses and Mineralogy of Lunar Mare Basalts Ages, Thicknesses and Mineralogy of Lunar Mare Basalts

Jan 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002mbns.conf...24h&link_type=abstract

The Moon Beyond 2002: Next Steps in Lunar Science and Exploration, p. 24

Physics

Lunar Maria, Lunar Surface, Cratering, Lunar Craters, Mineralogy, Petrogenesis, Environment Models

Scientific paper

About 17% of the lunar surface are covered with lunar mare basalts. Mare basalts occur preferentially on the lunar nearside and their presence on planetary surfaces is indicative of the thermal activity and volcanic evolution of the body. In order to place constraints on the thermal/volcanic evolution and petrogenetic models for the formation of lunar mare basalts, we dated basalts exposed on the lunar nearside. Over the last 6 years we performed crater counts for Oceanus Procellarum, Mare Nubium, Cognitum, Insularum, Humorum, Imbrium, Serenitatis, Tranquillitatis, Humboldtianum, and Australe. Currently we are extending our crater counts to basalt areas in Mare Frigoris, Nectaris, Vaporum, Smythii, and Marginis. We are also in the progress of dating some lava-filled impact craters such as Schickard, Cr?ger, and Grimaldi. Crater counts not only allow one to determine the age of a basalt unit but also provide important information about the thickness, the volume, and the temporal separation of individual basalt flow units. In addition, age data in combination with Clementine and Lunar Prospector data allow one to investigate changes in mineralogy with time.

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