The Dynamical Evolution of the Earth-Moon Progenitors

Details The Dynamical Evolution of the Earth-Moon Progenitors The Dynamical Evolution of the Earth-Moon Progenitors

Jan 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998lpico.957...38r&link_type=abstract

Origin of the Earth and Moon, Proceedings of the Conference held 1-3 December, 1998 in Monterey, California. LPI Contribution N

Other

Angular Momentum, Collisions, Earth-Moon System, Moon, Solar System, Terrestrial Planets, Many Body Problem, Computerized Simulation

Scientific paper

Substantial evidence indicates that the Earth-Moon system formed about 100 m.y. after the oldest meteorites and that the inner solar system had five terrestrial planets for several tens of millions of years before the hypothesized Moon-forming impact. We present and discuss some results from a series of N-body integrations in which the mass ratio of the Earth-Moon progenitors is 8:1 or 1:1. We want to know if it is plausible to have the Earth-Moon progenitors collide between 8 m.y. and 200 m.y. after the other planets had formed and to have the resulting system look "similar" to the solar system. If a collision occurs, the integrations tell us which two bodies collide and the time of the collision. We also determine the angular momentum deficit (AMD) of the resulting terrestrial planets. Additionally, we calculate several parameters of the collision. We use the AMD of the terrestrial planets to compare the resulting system to our own. The AMD or a planet is the difference between its orbital angular momentum and its orbital angular momentum if it were in a circular orbit with zero inclination.

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