Other
Scientific paper
Apr 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003eaeja.....4432k&link_type=abstract
EGS - AGU - EUG Joint Assembly, Abstracts from the meeting held in Nice, France, 6 - 11 April 2003, abstract #4432
Other
Scientific paper
The intense remanent magnetization of the Mars crust must be due to one or more of a very few candidate minerals. The most efficient magnetic minerals capable of producing stable magnetization on Mars are dispersed magnetite and pyrrhotite grains of less than 100 nm in diameter and dispersed (exsolved) hematite regardless of grain size. Larger magnetite and pyrrhotite grains (greater than 1000 nm) have large intrinsic demagnetizing fields causing low values of acquired remanence. Hematite has 2 orders of magnitude lower demagnetizing field, allowing preservation of SD -like behavior for grain diameters reaching 0.2 mm. The larger amplitude of magnetic anomalies on Mars relates either to larger volume or large magnetic density of the rocks that were magnetized in a uniform direction. The nature of the magnetic source could include intrusive and/or metamorphic rocks with predominantly coarse-grained granular texture. We analyzed hematite ilmenite series of exsolved minerals commonly found in deep crustal rocks on Earth. Finely exsolved titanohematite within ferrian ilmenite host and titanohematite with fine ferrian ilmenite exsolution both have sufficiently strong magnetization to explain magnetic anomalies on Mars. We also analyzed the mineral acquisition properties for magnetite and hematite, and found grain size regions that may allow amplification of the preexisting magnetization without the presence of the ambient magnetic field. This amplification depends on the nature of the thermal gradient across the Curie isotherm.
Acuña Mario Humberto
Connerney Jack E. P.
Kletetschka Gunther
Ness Norman F.
Wasilewski Peter J.
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