Lunar accretion from a Roche-interior fluid disk

Details Lunar accretion from a Roche-interior fluid disk Lunar accretion from a Roche-interior fluid disk

Oct 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011epsc.conf.1559s&link_type=abstract

EPSC-DPS Joint Meeting 2011, held 2-7 October 2011 in Nantes, France. http://meetings.copernicus.org/epsc-dps2011, p.1559

Physics

Scientific paper

We use a hybrid numerical approach to simulate the formation of the Moon from a circumterrestrial disk: a fluid disk to model the disk inside the Roche limit, and an N-body code for the outer particles. As the fluid disk spreads due to its viscosity, new material is delivered across the Roche limit and accreetes in moonlets that can then collide to form the Moon. Contrary to an accretion timescale of a few months obtained with pure N-body codes, the growth of the moon is here limited by the slow spreading of the inner disk, resulting in accretion timescales up to hundreds of years.

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