Matching Martian crustal magnetization and magnetic properties of Martian meteorites

Rochette, P.; Gattacceca, J.; Chevrier, V. F.; Hoffmann, V.; Lorand, Jean‐Pierre; Funaki, M.; Hochleitner, Rupert

doi:10.1111/j.1945-5100.2005.tb00961.x

Cited by 83 publications

(79 citation statements)

References 38 publications

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“…We do not discuss paleomagnetic studies of iron meteorites and pallasites due to their poorly understood magnetic field recording properties (e.g., Guskova 1965b;Brecher and Albright 1977;. We also do not discuss the extensive work in lunar (reviewed by Fuller 1974Fuller , 2007Hood and Cisowski 1983;Fuller and Cisowski 1987;Dunlop and Ozdemir 1997;Wieczorek et al 2006) and Martian paleomagnetism (see Rochette et al 2001Rochette et al , 2005Rochette et al , 2006Fuller 2007;Acuña et al 2008) except as they relate to the general context of extraterrestrial paleomagnetism. Although most work on meteorites took place in the 1970s and early 1980s (see previous reviews by Levy and Sonett 1978;Hood and Cisowski 1983;Collinson 1992Collinson , 1994Dunlop and Ozdemir 1997;Fuller 2007;Rochette et al 2009b), there has recently been a burst of activity brought on by advances in paleomagnetic techniques and instrumentation, an increasingly numerous and diverse sample suite, advances in dynamo theory, and perhaps most importantly, a growing petrologic and geochemical dataset that is providing crucial contextual and geochronological information for understanding the nature and origin of remanent magnetization.…”

Section: Introductionmentioning

confidence: 96%

Paleomagnetic Records of Meteorites and Early Planetesimal Differentiation

et al. 2009

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The large-scale compositional structures of planets are primarily established during early global differentiation. Advances in analytical geochemistry, the increasing diversity of extraterrestrial samples, and new paleomagnetic data are driving major changes in our understanding of the nature and timing of these early melting processes. In particular, paleomagnetic studies of chondritic and small-body achondritic meteorites have revealed a diversity of magnetic field records. New, more sensitive and highly automated paleomagnetic instrumentation and an improved understanding of meteorite magnetic properties and the effects of shock, weathering, and other secondary processes are permitting primary and secondary magnetization components to be distinguished with increasing confidence. New constraints on the post-accretional histories of meteorite parent bodies now suggest that, contrary to early expectations, few if any meteorites have been definitively shown to retain records of early solar and protoplanetary nebula magnetic fields. However, recent studies of pristine samples coupled with new theoretical insights into the possibility of dynamo generation on small bodies indicate that some meteorites retain records of internally generated fields. These results indicate that some planetesimals formed metallic cores and early dynamos within just a few million years of solar system formation.

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Section: Introductionmentioning

confidence: 96%

Paleomagnetic Records of Meteorites and Early Planetesimal Differentiation

et al. 2009

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“…Therefore, the maximum depth to the Curie isotherm for the above minerals ranges from $16 km for pyrrhotite to $33 km for hematite. Depending on grain size, all of the above minerals are capable of providing magnetization intensities of the required magnitudes [Kletetschka et al, 2003;Rochette et al, 2005].…”

Section: Demagnetization By Low-velocity Secondary Impactsmentioning

confidence: 99%

Impact demagnetization of the Martian crust: Primaries versus secondaries

Artemieva

Hood

Ivanov

2005

Geophysical Research Letters

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[1] Numerical simulations presented here show that demagnetization of crust near the largest Martian basins by secondary impacts can be comparable to that by direct shock waves outside the transient cavity. The relative input from secondary impacts, which demagnetize only the uppermost layers, depends on the magnetic carrier distribution within the crust. Thus, we discuss properties of likely magnetic remanence carriers and their possible spatial distribution within the crust. Citation: Artemieva, N., Hood, and B. A. Ivanov (2005), Impact demagnetization of the Martian crust: Primaries versus secondaries, Geophys. Res. Lett., 32, L22204,

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“…However, this depth is rather arbitrary and actually depends on the magnetic mineral carrying the remanence and the crustal temperature gradient at the time of dynamo shutdown (see discussion in Kletetschka et al, 2000;Rochette et al, 2001Rochette et al, , 2005Dunlop and Arkhani-Ahmed, 2005). Spatial variations in this steady field can be used to delineate the NRM direction and intensity of subsurface formations.…”

Section: Application Of Surface Magnetic Field Measurementsmentioning

confidence: 98%

“…Indeed, the large magnetic field pulse associated with lightning current induces a large isothermal remanent magnetization (IRM). According to a survey of martian meteorites, the expected range of saturation IRM is 10-1,000 A/m (Rochette et al, 2005). Lightning NRM is usually a few tenths of saturation IRM (Wasilewsky and Dickinson, 2000;Verrier and Rochette, 2002).…”

Section: Application Of Surface Magnetic Field Measurementsmentioning

confidence: 99%

“…According to SNC studies (e.g., Rochette et al, 2001Rochette et al, , 2005Lorand et al, 2005), the major ironrich phases in these rocks are sulfides (mostly pyrrhotite FeS 1-x ) and titanomagnetite (Fe 3-x Ti x O 4 ). According to mass balance estimations, up to 10-30% of the regolith mass could be due to meteoritic bombardment (Flynn and McKay, 1990).…”

Section: Iron Minerals In Martian Regolithmentioning

confidence: 99%

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Magnetism, Iron Minerals, and Life on Mars

et al. 2006

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A short critical review is provided on two questions linking magnetism and possible early life on Mars: (1) Did Mars have an Earth-like internal magnetic field, and, if so, during which period and was it a requisite for life? (2) Is there a connection between iron minerals in the martian regolith and life? We also discuss the possible astrobiological implications of magnetic measurements at the surface of Mars using two proposed instruments. A magnetic remanence device based on magnetic field measurements can be used to identify Noachian age rocks and lightning impacts. A contact magnetic susceptibility probe can be used to investigate weathering rinds on martian rocks and identify meteorites among the small regolith rocks. Both materials are considered possible specific niches for microorganisms and, thus, potential astrobiological targets. Experimental results on analogues are presented to support the suitability of such in situ measurements.

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Matching Martian crustal magnetization and magnetic properties of Martian meteorites

Cited by 83 publications

References 38 publications

Paleomagnetic Records of Meteorites and Early Planetesimal Differentiation

Paleomagnetic Records of Meteorites and Early Planetesimal Differentiation

Impact demagnetization of the Martian crust: Primaries versus secondaries

Magnetism, Iron Minerals, and Life on Mars

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