Building Terrestrial Planets
Building Terrestrial Planets
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DOI：
10.1146/annurev-earth-042711-105319
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发表时间：
2012-05
影响因子：
14.9
通讯作者：
A. Morbidelli;J. Lunine;David P. Obrien;S. Raymond;K. Walsh
中科院分区：
文献类型：
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作者：
A. Morbidelli;J. Lunine;David P. Obrien;S. Raymond;K. Walsh
本文回顾了我们目前对类地行星形成的认识。重点是吸积过程的动力学方面的计算机模拟。在整个审查中，我们结合联合收割机的结果，这些理论模型与地球化学，宇宙化学和年代学的限制，概述了我们的太阳系的早期演化的综合方案。鉴于巨行星首先形成于原行星盘，我们强调类地行星吸积过程对巨行星轨道结构及其演化的敏感依赖性。这表明在太阳系外的类地行星种群中存在着巨大的多样性。深入讨论了火星和地球之间不同质量和吸积时间尺度的原因以及我们星球上水（和其他挥发物）的起源等问题。
This article reviews our current understanding of terrestrial planet formation. The focus is on computer simulations of the dynamical aspects of the accretion process. Throughout the review, we combine the results of these theoretical models with geochemical, cosmochemical, and chronological constraints to outline a comprehensive scenario of the early evolution of our solar system. Given that the giant planets formed first in the protoplanetary disk, we stress the sensitive dependence of the terrestrial planet accretion process on the orbital architecture of the giant planets and on their evolution. This suggests a great diversity among the terrestrial planet populations in extrasolar systems. Issues such as the cause for the different masses and accretion timescales between Mars and Earth and the origin of water (and other volatiles) on our planet are discussed in depth.