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Simulations for Terrestrial Planets Formation

Published online by Cambridge University Press:  06 April 2010

Jianghui Ji  and
Niu Zhang
Jianghui Ji
Affiliation:
Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210008, China email: jijh@pmo.ac.cn
Niu Zhang
Affiliation:
Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210008, China email: jijh@pmo.ac.cn Graduate School of Chinese Academy of Science, Beijing 100049
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Abstract

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We investigate the formation of terrestrial planets in the late stage of planetary formation using two-planet model. At that time, the protostar has formed for about 3 Myr and the gas disk has dissipated. In the model, the perturbations from Jupiter and Saturn are considered. We also consider variations of the mass of outer planet, and the initial eccentricities and inclinations of embryos and planetesimals. Our results show that, terrestrial planets are formed in 50 Myr, and the accretion rate is about 60% - 80%. In each simulation, 3 - 4 terrestrial planets are formed inside “Jupiter” with masses of 0.15 – 3.6 M⊕. In the 0.5 - 4AU, when the eccentricities of planetesimals are excited, planetesimals are able to accrete material from wide radial direction. The plenty of water material of the terrestrial planet in the Habitable Zone may be transferred from the farther places by this mechanism. Accretion may also happen a few times between two giant planets only if the outer planet has a moderate mass and the small terrestrial planet could survive at some resonances over time scale of 108 yr.

Keywords

methods:n-body simulations-planetary systems-planetary formation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S263: Icy Bodies of the Solar System , August 2009 , pp. 45 - 49
Copyright
Copyright © International Astronomical Union 2010

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