Document Type
Article
Publication Date
1979
Abstract
The norphology of peak/pit tructures in craters on Mars does no t appear to be controlled by the terrain, type (plains units or cratered terrain). The formation of these simple central peaks, central peaks with small sumnit pits, massive central peats with large summit pits, or nearly rimless central pits, may be sensitive to the characteristics of the consoli- dated substrate, and particularly to the amount of volatiles trapped in it. pits of the equatorial region of Concentration of central in craters Mars indicates that considerable anoun-s of volatiles are trapped under the plains units. On the ruggcd terrair, the occurrance of simple peaks in large craters may be caused by lack of volatiles in the original units or the escape of volatile constitucnts during meteorite impacts. The simple peaks appear to be more resistant to degradation than central pits. The orientation of young, elongate crater rims on Mars indicates a global structurel control, while those of the old crater rins may bo explained by a weaker structural trend in a NE-S₩ direction or by preferential obliquity of early impacts.
Recommended Citation
El-Baz, Farouk, "Distribution and orientation of peak-pit structure in martian craters" (1979). Farouk El-Baz Library. 69.
https://buescholar.bue.edu.eg/farouk_el-baz_library/69