The migration of volatiles on the surfaces of Mercury and the Moon
The migration of volatiles on the surfaces of Mercury and the Moon
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DOI：
10.1029/97je01347
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发表时间：
1997-08
影响因子：
--
通讯作者：
B. Butler
中科院分区：
文献类型：
--
作者：
B. Butler
对水星的雷达观测提供了一个惊人的发现，即在永久阴影的极地地区可能存在大量的冰沉积物[Butler等人，1993；哈蒙等人，1994]。这重新引发了关于月球极地地区存在这种沉积物的旧争论。为了建立这样的沉积物，挥发物很可能必须能够迁移到这些天体的极地地区。本文介绍了Butler等人[1993]对水星表面分子迁移的蒙特卡罗模拟的扩展结果。模拟结果表明，在水星的典型条件下，随机放置在表面的所有h2o的~ 5-15%迁移到稳定（永久阴影）的极地地区。对于月球来说，这个数字是20-50%。二氧化碳迁移的数字在水星为~ 2%，在月球为~ 13%。这些百分比与之前的计算结果相似，支持了水星和月球两极地区存在冰沉积的观点。
Radar observations of Mercury have provided the startling discovery of the probable existence of substantial deposits of ices in permanently shaded polar regions [Butler et al., 1993; Harmon et al., 1994]. This has renewed the old argument about the existence of such deposits in the polar regions of the Moon. It is most likely necessary for volatiles to be able to migrate to the polar regions of these bodies in order to build up such deposits. This paper presents the results of the extension of a Monte Carlo simulation of the migration of molecules on the surface of Mercury by Butler et al. [1993]. The results of the simulations show that for typical conditions on Mercury, ∼5-15% of all H 2 O which is placed randomly on the surface migrates to stable (permanently shaded) polar regions. For the Moon the numbers are ∼ 20-50%. The numbers for the migration of CO 2 are ∼2% for Mercury and ∼13% for the Moon. These percentages are similar to those previously calculated and support the idea of ice deposits in the polar regions of both Mercury and the Moon.