The Martian impact cratering record.
The Martian impact cratering record.
复制标题
火星撞击坑的记录。
DOI：
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发表时间：
1992
期刊：
影响因子：
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通讯作者：
N. Barlow
中科院分区：
文献类型：
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作者：
R. Strom;S. Croft;N. Barlow
详细分析了火星撞击坑的记录。火星与月球和水星在撞击坑形态和形态测量学上的主要差异被认为主要是火星地表下挥发物的结果。一般来说，这些挥发物的深度可能会随着南半球纬度的增加而减少，但这一层的底部可能或多或少处于恒定的深度。Martial地壳的二分法可能是火星吸积接近尾声时一次非常大的撞击的结果。蒙特卡洛计算机模拟表明，这种影响不仅是可能的，而且很可能。火星高地的陨石坑记录显示，相对于月球高地，直径小于30公里的陨石坑非常少。陨石坑的稀少可能是早期强烈的侵蚀和风成、河流和冰川作用造成的沉积作用造成的。
A detailed analysis of the Martian impact cratering record is presented. The major differences in impact crater morphology and morphometry between Mars and the moon and Mercury are argued to be largely the result of subsurface volatiles on Mars. In general, the depth to these volatiles may decrease with increasing latitude in the southern hemisphere, but the base of this layer may be at a more or less constant depth. The Martial crustal dichotomy could have been the result of a very large impact near the end of the accretion of Mars. Monte Carlo computer simulations suggest that such an impact was not only possible, but likely. The Martian highland cratering record shows a marked paucity of craters less than about 30 km in diameter relative to the lunar highlands. This paucity of craters was probably the result of the obliteration of craters by an early period of intense erosion and deposition by aeolian, fluvial, and glacial processes.