[77.02] Dynamical Simulations of Terrestrial Planet Formation During Giant Planet Migration

AAS 207th Meeting, 8-12 January 2006
Session 77 From Hot Jupiters to Hot Earths
Poster, Tuesday, 9:20am-6:30pm, January 10, 2006, Exhibit Hall

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[77.02] Dynamical Simulations of Terrestrial Planet Formation During Giant Planet Migration

A. M. Mandell (PSU/PSARC/GSFC), S. N. Raymond (Colorado/VPL), S. Sigurdsson (PSU/PSARC)

We present preliminary results of dynamical simulations of young planetary systems undergoing migration of a Jovian-type planet through the terrestrial region. We find that a significant fraction (10-40%) of the initial planetary embryos remain after giant planet migration, and subsequent evolution of the system results in the formation of terrestrial planets in various configurations, often including a planet in the Habitable Zone. In simulations with gas drag, 3-6 Earth mass planets are formed interior to the migrating Jovian planet, swept inward through moving resonances, and eccentricities are damped for all planets. Systematic variations are seen between simulations with and without gas drag. The presence of a second, non-migrating giant planet reduces the water content and mass of the planets formed throughout the system.

This research was supported in part by the Penn State Astrobiology Research Center and the Goddard Center for Astrobiology.

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