Origin of water in the inner Solar System: A kinetic Monte Carlo study of water adsorption on forsterite
Origin of water in the inner Solar System: A kinetic Monte Carlo study of water adsorption on forsterite
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DOI：
10.1016/j.icarus.2008.07.017
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发表时间：
2008-12-01
期刊：
影响因子：
3.2
通讯作者：
Drake, Michael J.
中科院分区：
文献类型：
--
作者：
Muralidharan, Krishna;Deymier, Pierre;Drake, Michael J.
内太阳系中水的起源还没有被很好地理解。据信，在类地行星区域的吸积盘中，温度太高，含水相不可能是热力学稳定的。水的来源包括类地行星形成后，星云中的氢直接吸附到岩浆海洋中，以及来自类地行星带以外的小行星或彗星物质。我们探索了一个新的想法，在行星吸积之前直接将水吸附到颗粒上。这一假说的动机是观察到，我们的行星系统形成的吸积盘是由固体颗粒组成的，这些颗粒沐浴在以氢、氦和氧为主的气体中。其中一些氢和氧化合成水蒸气。我们研究定量吸附水颗粒在太阳系内吸积盘通过探索水分子的吸附动力学到镁橄榄石表面通过动力学蒙特卡罗模拟。我们的结论是，地球上许多海洋的水可以被吸附。(C)2008年爱思唯尔公司All rights reserved.
The origin of water in the inner Solar System is not well understood. It is believed that temperatures were too high in the accretion disk in the region of the terrestrial planets for hydrous phases to be thermodynamically stable. Suggested Sources of water include direct adsorption of hydrogen from the nebula into magma oceans after the terrestrial planets formed, and delivery of asteroidal or cometary material from beyond the zone of the terrestrial planets. We explore a new idea, direct adsorption of water onto grains prior to planetary accretion. This hypothesis is motivated by the observation that the accretion disk from which our planetary system formed was composed of solid grains bathed in a gas dominated by hydrogen, helium, and oxygen. Some of that hydrogen and oxygen combined to make water vapor. We examine quantitatively adsorption of water onto grains in the inner Solar System accretion disk by exploring the adsorption dynamics of water molecules onto forsterite surfaces via kinetic Monte Carlo simulations. We conclude that many Earth oceans of water could be adsorbed. (C) 2008 Elsevier Inc. All rights reserved.