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The Formation of Planets Around Stars of Various Masses and the Origin and the Evolution of Circumstellar Dust Clouds

Published online by Cambridge University Press:  04 August 2017

Takenori Nakano
Takenori Nakano*
Affiliation:
Department of Physics, Kyoto University, Sakyo-ku, Kyoto 606, Japan

Abstract

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The formation of planets is investigated both in a gaseous nebula and after the nebula has been blown away. The capture of planetesimals by a protoplanet is investigated by taking into account the growth of planetesimals. The time of planet formation is determined as a function of distance from the central star. The formation time of Neptune is found to be 3.9 × 109 yr, value shorter than the age of the solar system. The region where planets form within the stellar lifetime is determined, and it is found that only stars of mass less than several solar masses can have planets. The dust clouds around α Lyrae and β Pictoris are far outside the planet-forming regions. A model for the circumstellar dust cloud is proposed which can explain the basic properties of the β Pic disk.

Type
I. Star Forming Processes in the Solar Neighborhood
Information
Symposium - International Astronomical Union , Volume 115: Star Forming Regions , 1987 , pp. 301 - 313
Copyright
Copyright © Reidel 1987 

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