AN INTRODUCTION TO MARTIAN GRID SYSTEM

被引：4

作者：

WELLS, RA

机构：

[1] University of London Observatory, London, N W. 7., Mill Hill Park

来源：

GEOPHYSICAL JOURNAL OF THE ROYAL ASTRONOMICAL SOCIETY | 1969年 / 17卷 / 02期

关键词：

D O I：

10.1111/j.1365-246X.1969.tb02322.x

中图分类号：

P3 [地球物理学]; P59 [地球化学];

学科分类号：

0708 ; 070902 ;

摘要：

The linear features on Mars, commonly referred to as canals, have been mapped into two overlapping grid patterns‐one oriented approximately NW‐SE, NE‐SW, and the other N‐S, ECW. The tectonic aspects of the lineaments are discussed and comparisons of the grid patterns are made with the lunar grid system. These lineaments have been deduced to be tectonic zones of weakness. The grid patterns on Mars can be mapped through 360° of longitude. Similarities in the lunar and Martian diagonal grids suggest a similar origin for both systems. The presence of a N‐S, E‐W grid for Mars and the absence of one for the Moon indicates differences in tectonic activity between the lunar and Martian crusts. Copyright © 1969, Wiley Blackwell. All rights reserved

引用

页码：209 / &

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