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The Magnetism of Meteorites and Early Solar System Magnetic Fields [and Discussion]
D. W. Collinson, R. Hide, R. Hutchison and S. K. Runcorn
Philosophical Transactions: Physical Sciences and Engineering
Vol. 349, No. 1690, The Solar-System: A Review of Results from Space Missions (Nov. 15, 1994), pp. 197-207
Published by: Royal Society
Stable URL: http://www.jstor.org/stable/54252
Page Count: 11
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The characteristics of the remanent magnetization of chondrite, achondrite and shergottite, nakhlite and chassignite (SNC) meteorites are described, and interpretation in terms of magnetizing fields in the ancient Solar System discussed. The magnetism of ordinary chondrites is commonly scattered in direction within samples, implying magnetization of constituent fragments before accumulation. The magnetic history of these meteorites is uncertain because of lack of knowledge of the origin and properties of tetrataenite, an ordered FeNi alloy often carrying the bulk of the magnetization. Achondrites also often possess scattered magnetization, the primary component probably being acquired during cooling after differentiation of the parent body. A magnetizing field of internal origin is possible. Estimates of magnetizing field strength are in the approximate range 5-100 μ T, with carbonaceous chondrites showing the highest values. The SNC meteorites, probably originating on Mars, provide evidence for a weak, ancient Martian magnetic field of the order 1 μ T.
Philosophical Transactions: Physical Sciences and Engineering © 1994 Royal Society