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- Francis Nimmo
- Department of Earth and Space Sciences, University of California, Los Angeles, California 90095-1567;
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- Ken Tanaka
- United States Geological Survey, Flagstaff, Arizona 86001;
書誌事項
- 公開日
- 2005-05-31
- DOI
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- 10.1146/annurev.earth.33.092203.122637
- 公開者
- Annual Reviews
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説明
<jats:p>▪ Abstract The bulk of the ∼50-km-thick Martian crust formed at ∼4.5 Gyr B.P., perhaps from a magma ocean. This crust is probably a basaltic andesite or andesite and is enriched in incompatible and heat-producing elements. Later additions of denser basalt to the crust were volumetrically minor, but resurfaced significant portions of the Northern hemisphere. A significant fraction of the total thickness of the crust was magnetized prior to 4 Gyr B.P., with the magnetization later selectively removed by large impacts. Early large impacts also modified the hemispheric contrast in crustal thickness (the dichotomy), which was possibly caused by long-wavelength mantle convection. Subsequent Noachian modification of the crust included further impacts, significant fluvial erosion, and volcanism associated with the formation of the Tharsis rise. Remaining outstanding questions include the origin of the dichotomy and the nature of the magnetic anomalies.</jats:p>
収録刊行物
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- Annual Review of Earth and Planetary Sciences
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Annual Review of Earth and Planetary Sciences 33 (1), 133-161, 2005-05-31
Annual Reviews
