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Formation of terrestrial planets

Published online by Cambridge University Press:  13 January 2020

Eiichiro Kokubo Open the ORCID record for Eiichiro Kokubo [Opens in a new window]
Eiichiro Kokubo*
Affiliation:
National Astronomical Observatory of Japan, 2-21-1, Osawa, Mitaka, 181-8588Japan, email: kokubo.eiichiro@nao.ac.jp
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Abstract

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In the standard formation scenario of planetary systems, planets form from a protoplanetary disk that consists of gas and dust. The scenario can be divided into three stages: (1) formation of planetesimals from dust, (2) formation of protoplanets from planetesimals, and (3) formation of planets from protoplanets. In stage (1), planetesimals form from dust through coagulation of dust grains and/or some instability of a dust layer. Planetesimals grow by mutual collisions to protoplanets or planetary embryos through runaway and oligarchic growth in stage (2). The final stage (3) of terrestrial planet formation is giant impacts among protoplanets while sweeping residual planetesimals. In the present paper, we review the elementary processes of terrestrial planet formation and discuss the extension of the standard scenario.

Keywords

solar system: formationplanets and satellites: formation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S345: Origins: From the Protosun to the First Steps of Life , August 2018 , pp. 141 - 147
Copyright
© International Astronomical Union 2020 

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