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Theoretical predictions of mass, semimajor axis and eccentricity distributions of super-Earths

Published online by Cambridge University Press:  10 November 2011

Shigeru Ida
Shigeru Ida*
Affiliation:
Department of Earth & Planetary Science, Tokyo Institute of Technology, Ookayama 2-12-1 I2-10, Tokyo 152-8551, Japan email: ida@geo.titech.ac.jp
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Abstract

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We discuss the effects of close scattering and merging between planets on distributions of mass, semimajor axis and orbital eccentricity, using population synthesis model of planet formation, focusing on the distributions of close-in super-Earths, which are being observed recently. We found that a group of compact embryos emerge interior to the ice line, grow, migrate, and congregate into closely-packed convoys which stall in the proximity of their host stars. After the disk-gas depletion, they undergo orbit crossing, close scattering, and giant impacts to form multiple rocky Earths or super-Earths in non-resonant orbits around ~ 0.1AU with moderate eccentricities of ~ 0.01–0.1. The formation of these planets does not depend on model parameters such as type I migration speed. The fraction of solar-type stars with these super-Earths is anti-correlated with the fraction of stars with gas giants. The newly predicted family of close-in super-Earths makes less clear “planet desert” at intermediate mass range than our previous prediction.

Keywords

planets and satellites: dynamical evolution and stabilityplanets and satellites: formationplanetary systems: protoplanetary disks
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S276: The Astrophysics of Planetary Systems: Formation, Structure, and Dynamical Evolution , October 2010 , pp. 64 - 71
Copyright
Copyright © International Astronomical Union 2011

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