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Orbital migration and mass-semimajor axis distributions of extrasolar planets

Published online by Cambridge University Press:  01 October 2007

Shigeru Ida  and
D. N. C. Lin
Shigeru Ida
Affiliation:
Tokyo Institute of Technology, Ookayama, Meguro-ku, Tokyo 152-8551, Japan email: ida@geo.titech.ac.jp
D. N. C. Lin
Affiliation:
UCO/Lick Observatory, University of California, Santa Cruz, CA 95064, USA Kavli Institute of Astronomy & Astrophysics, Peking University, Beijing, China email: lin@ucolick.org
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Abstract

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Here we discuss the effects of type-I migration of protoplanetary embryos on mass and semimajor axis distributions of extrasolar planets. We summarize the results of Ida & Lin (2008a, 2008b), in which Monte Carlo simulations with a deterministic planet-formation model were carried out. The strength of type-I migration regulates the distribution of extrasolar gas giant planets as well as terrestrial planets. To be consistent with the existing observational data of extrasolar gas giants, the type-I migration speed has to be an order of magnitude slower than that given by the linear theory. The introduction of type-I migration inhibits in situ formation of gas giants in habitable zones (HZs) and reduces the probability of passage of gas giants through HZs, both of which facilitate retention of terrestrial planets in HZs. We also point out that the effect of magneto-rotational instability (MRI) could lead to trapping of migrating protoplanetary embryos in the regions near an ice line in the disk and it significantly enhances formation/retention probability of gas giants against type-I migration.

Keywords

planetary systems: formationsolar system: formationstars: statics
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S249: Exoplanets: Detection, Formation and Dynamics , October 2007 , pp. 223 - 232
Copyright
Copyright © International Astronomical Union 2008

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