Seismic models of the Moon: constraints in mineralogy, temperature andimpact formation

Details Seismic models of the Moon: constraints in mineralogy, temperature andimpact formation Seismic models of the Moon: constraints in mineralogy, temperature andimpact formation

Apr 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003eaeja....10285l&link_type=abstract

EGS - AGU - EUG Joint Assembly, Abstracts from the meeting held in Nice, France, 6 - 11 April 2003, abstract #10285

Computer Science

Scientific paper

We use a seismic model of the Moon as well as the Clementine and Lunar Prospector value of the moment of Inertia to constrain the mineralogy and temperature of the Moon mantle. The seismic model was obtained from a complete reprocessing of the Apollo data, leading to a new set of arrival time with associated errors. Both the travel times of shallow and deep moonquakes, as well as those from artificial and meteoritic impacts were used. In addition, receiver function amplitudes were used for the crust at the Apollo 12 landing site. In the Procellarum KREEP Terrane, the only major discontinuity compatible with the crust-mantle boundary found is located around 30 km deep. Seismic constraints on the crust and mantle lead to a 30 km thick anorthositic crust and a pyroxenite cold mantle, of bulk composition 6.4% in Al2O3, 4.9% in CaO, and 13.3 % in FeO. Mantle temperatures are in accordance with profiles obtained from the observed electrical conductivity and exclude a liquid Fe core, while being compatible with a Fe-S liquid core. Our Moon model might be explained by a mixture between a primitive Earth with tholeiitic crust and depleted upper mantle, and a chondritic enstatic parent body for the impactor planet. The high U content of the Moon can be explained by the significant part of the tholeitic crust ejected from the Earth during the primordial impact. The values found by our model for the ejected crust are comparable to those obtained by impact simulations.

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