Distribution of small channels on the Martian surface
Distribution of small channels on the Martian surface
复制标题
火星表面小水道的分布
DOI：
10.1016/0019-1035(76)90182-2
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发表时间：
1976
期刊：
影响因子：
3.2
通讯作者：
D. Pieri
中科院分区：
文献类型：
--
作者：
D. Pieri
火星上小通道的分布已经从水手9号图像中绘制出来，比例尺为1：5000000。这里所指的小通道是一些小山谷，宽度从水手9号广角图像的分辨率极限（101公里）到大约10公里不等。最大密度的小带出现在黑暗的陨石坑地形。这个暗区形成了一个环绕地球的广阔的近赤道带。观测到的分布可能是由于高密度尘埃或沉积物地幔的遮蔽导致明亮区域小通道能见度降低的结果。两个小通道段内的陨石坑密度显示陨石坑的大小频率分布与最古老的重陨石坑平原单位一致。这样的陨石坑密度，再加上在旧的陨石坑地形中几乎只出现小通道，以及高分辨率图像（100米）中小通道的外观普遍退化，意味着火星地质历史早期小通道形成的主要情节。
The distribution of small channels on Mars has been mapped from Mariner 9 images, at the 1:5 000 000 scale, by the author. The small channels referred to here are small valleys ranging in width from the resolution limit of the Mariner 9 wide-angle images (∼1 km) to about 10 km. The greatest density of small band occurs in dark cratered terrain. This dark zone forms a broad subequatorial band around the planet. The observed distribution may be the result of decreased small-channel visibility in bright areas due to obscuration by a high albedo dust or sediment mantle. Crater densities within two small-channel segments show crater size-frequency distributions consistent with those of the oldest of the heavily cratered plains units. Such crater densities coupled with the almost exclusive occurrence of small channels in old cratered terrain and the generally degraded appearance of small channels in the high-resolution images (∼100 m) imply a major episode of small-channel formation early in Martian geologic history.