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Terrestrial Planet Formation: The Solar System and Other Systems

Published online by Cambridge University Press:  26 May 2016

Shigeru Ida  and
Eiichiro Kokubo
Shigeru Ida
Affiliation:
Tokyo Institute of Technology, Meguro-ku, Tokyo 158-5881, Japan
Eiichiro Kokubo
Affiliation:
National Astronomical Observatory, Mitaka-shi, Tokyo 181-8588, Japan

Abstract

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Accretion of terrestrial planets and solid cores of jovian planets is discussed, based on the results of our N-body simulations. Protoplanets accrete from planetesimals through runaway and oligarchic growth until they become isolated. The isolation mass of protoplanets in terrestrial planet region is about 0.2 Earth mass, which suggests that in the final stage of terrestrial planet formation giant impacts between the protoplanets occur. On the other hand, the isolation mass in jovian planet region is about a few to 10 Earth masses, which may be massive enough to form a gas giant. Extending the above arguments to disks with various initial masses, we discuss diversity of planetary systems. We predict that the extrasolar planets so far discovered may correspond to the systems formed from disks with large initial masses and that the other disks with smaller masses, which are the majority of the disks, may form Earth-like planets.

Type
Part II: Progress in the theory of planet formation
Information
Symposium - International Astronomical Union , Volume 202: Planetary Systems in the Universe – Observation, Formation and Evolution , 2004 , pp. 159 - 166
Copyright
Copyright © Astronomical Society of the Pacific 2004 

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