Pyrrhotite and the remanent magnetization of SNC meteorites: a changing perspective on Martian magnetism

By P. Rochette, J. Lorand, G. Fillion, V. Sautter. 2001

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Toward a robust normalized magnetic paleointensity method applied to meteorites (2004, methodology): “The magnetic remanence carriers of the studied meteorites are all suitable for the use of the REMV method: FeNi alloys for ordinary chondrites, aubrites, eucrites and diogenites; pyrrhotite or magnetite for Martian meteorites [12,26]; pyrrhotite for Rumuruti chondrites where opaque mineralogy studie”
EARLY CRUSTAL EVOLUTION OF MARS 1 (2005, background): “Martian meteorites typically contain titanomagnetite (Weiss et al. 2002) or pyrrhotite (Rochette et al. 2001).”
Paleomagnetic Records of Meteorites and Early Planetesimal Differentiation (2010, background): “Pyrrhotite has a magnetic phase transition at ∼2.8 GPa (Rochette et al. 2003a), meaning that pyrrhotite-bearing meteorites shocked above this pressures may have lost all or much of the record of their pre-shock remanent magnetization (Rochette et al. 2001; Louzada et al. 2007).”
Records of an ancient Martian magnetic field in ALH84001 (2001, background): “6 GPa for magnetite and pyrrhotite, respectively [9,52]) which might otherwise alter their primary 4 Ga remanence.”