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Eugenio Rivera (SUNY, Stony Brook), Jack J. Lissauer (NASA Ames), Martin J. Duncan (Queen's U., Kingston, ON), Harold F. Levison (SWRI)
To simulate the dynamics of the Solar System before the hypothesized Moon-forming impact, we are integrating the Solar System with the Earth-Moon system replaced by two bodies in heliocentric orbits between Venus and Mars. Their total (orbital) angular momentum is that of the present Earth-Moon system, and their total mass is that of the Earth-Moon system. We are looking at ranges in mass ratio and initial values for eccentricity, inclination, and semi-major axis. We are using the SYMBA integrator to integrate these systems until a collision occurs or a time of 200 Myr elapses. In this poster we present and discuss some results from a series of runs in which the mass ratio is 8:1, the initial inclination of the more massive body with respect to the ecliptic is 2/3\circ, the initial eccentricity of the more massive body is either 0.00 or 0.05, and the initial semi-major axis of the less massive body varies between 0.80 AU and 1.40 AU.
The author(s) of this abstract have provided an email address for comments about the abstract: rivera@epimethius.arc.nasa.gov