Rocks of the Columbia Hills

被引:131
作者
Squyres, Steven W.
Arvidson, Raymond E.
Blaney, Diana L.
Clark, Benton C.
Crumpler, Larry
Farrand, William H.
Gorevan, Stephen
Herkenhoff, Kenneth E.
Hurowitz, Joel
Kusack, Alastair
McSween, Harry Y.
Ming, Douglas W.
Morris, Richard V.
Ruff, Steven W.
Wang, Alian
Yen, Albert
机构
[1] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA
[2] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA
[3] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA
[4] Lockheed Martin Corp, Littleton, CO 80127 USA
[5] New Mexico Museum Nat Hist & Sci, Albuquerque, NM 87104 USA
[6] Space Sci Inst, Boulder, CO 80301 USA
[7] Honeybee Robot, New York, NY 10001 USA
[8] US Geol Survey, Flagstaff, AZ 86001 USA
[9] SUNY Stony Brook, Dept Geosci, Stony Brook, NY 11794 USA
[10] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA
[11] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA
[12] Arizona State Univ, Dept Geol Sci, Tempe, AZ 85287 USA
关键词
D O I
10.1029/2005JE002562
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
[ 1] The Mars Exploration Rover Spirit has identified five distinct rock types in the Columbia Hills of Gusev crater. Clovis Class rock is a poorly sorted clastic rock that has undergone substantial aqueous alteration. We interpret it to be aqueously altered ejecta deposits formed by impacts into basaltic materials. Wishstone Class rock is also a poorly sorted clastic rock that has a distinctive chemical composition that is high in Ti and P and low in Cr. Wishstone Class rock may be pyroclastic or impact in origin. Peace Class rock is a sedimentary material composed of ultramafic sand grains cemented by significant quantities of Mg- and Ca-sulfates. Peace Class rock may have formed when water briefly saturated the ultramafic sands and evaporated to allow precipitation of the sulfates. Watchtower Class rocks are similar chemically to Wishstone Class rocks and have undergone widely varying degrees of near-isochemical aqueous alteration. They may also be ejecta deposits, formed by impacts into Wishstone-rich materials and altered by small amounts of water. Backstay Class rocks are basalt/trachybasalt lavas that were emplaced in the Columbia Hills after the other rock classes were, either as impact ejecta or by localized volcanic activity. The geologic record preserved in the rocks of the Columbia Hills reveals a period very early in Martian history in which volcanic materials were widespread, impact was a dominant process, and water was commonly present.
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页数:19
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