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Szablon:Rochette (magnetic susceptibility, MaPS)

Z Wiki.Meteoritica.pl

1

Podstawowa literatura dotycząca podatności magnetycznej χ (ang. magnetic susceptibility) w zastosowaniu do klasyfikacji meteorytów kamiennych:

  • Rochette Pierre, Sagnotti Leonardo, Bourot-Denise Michèle, Consolmagno Guy, Folco Luigi, Gattacceca Jérôme, Osete Maria Luisa, Pesonen Lauri, (2003), Magnetic classification of stony meteorites: 1. Ordinary chondrites, Meteoritics & Planetary Science, vol. 38(2), 2003, s. 251-268 (→ więcej).[1] Plik doi.
  • Rochette Pierre, Gattacceca Jérôme, Bonal Lydie, Bourot-Denise Michèle, Chevrier Vincent, Clerc Jean-Pierre, Consolmagno Guy, Folco Luigi, Gounelle Matthieu, Kohout Tomas, Pesonen Lauri, Quirico Eric, Sagnotti Leonardo, Skripnik Anna, (2008), Magnetic classification of stony meteorites: 2. Non-ordinary chondrites, Meteoritics & Planetary Science, vol. 43(5), 2008, s. 959-980.[2] Plik doi.
  • Rochette Pierre, Gattacceca Jérôme, Bourot-Denise Michèle, Consolmagno Guy, Folco Luigi, Kohout Tomas, Pesonen Lauri, Sagnotti Leonardo, (2009), Magnetic classification of stony meteorites: 3. Achondrites, Meteoritics & Planetary Science, vol. 44(3), 2009, s. 405-427.[3] Plik doi.



Wykres wartości podatności magnetycznej (ang. magnetic susceptibility) dla meteorytów i wybranych skał ziemskich

Rochette et al. 2008: Mean magnetic susceptibility (logχ with χ in 10−9 m3/kg) for the different studied groups, compared to ordinary chondrite groups. Falls only are used for OC, CO3, and E chondrites

Rochette et al. 2009: Mean logχ (in 10−9 m3/kg) for the different studied achondrite groups, compared to selected chondrite groups. Meteorites excluded from the mean appear with crosses. Falls only are used for OC, CO3 and E (after Rochette et al. 2008). The metal amount (wt%) indicated is a maximum value, assuming non interacting multidomain spheres and not taking into account paramagnetic susceptibility

Przypisy

  1. ^ Abstract: We present a database of magnetic susceptibility measurements on 971 ordinary chondrites. It demonstrates that this parameter can be successfully used to characterize and classify ordinary chondrite meteorites. In ordinary chondrites, this rapid and non-destructive measurement essentially determines the amount of metal in the sample, which occurs in a very narrow range for each chondrite class (though terrestrial weathering can result in a variable decrease in susceptibility, especially in finds). This technique is particularly useful not only for a rapid classification of new meteorites, but also as a check against curation errors in large collections (i.e., unweathered meteorites, the measured susceptibility of which lies outside the expected range, may well be misclassified or misidentified samples). Magnetic remanence, related to magnetic field measurements around asteroids, is also discussed.
  2. ^ Abstract: A database of magnetic susceptibility (χ) measurements on different non-ordinary chondrites (C, E, R, and ungrouped) populations is presented and compared to our previous similar work on ordinary chondrites. It provides an exhaustive study of the amount of iron-nickel magnetic phases (essentially metal and magnetite) in these meteorites. In contrast with all the other classes, CM and CV show a wide range of magnetic mineral content, with a two orders of magnitude variation of χ. Whether this is due to primary parent body differences, metamorphism or alteration, remains unclear. C3–4 and C2 yield similar χ values to the ones shown by CK and CM, respectively. By order of increasing χ, the classes with well-grouped χ are: R << CO < CK ≈ CI < Kak < CR < E ≈ CH < CB. Based on magnetism, EH and EL classes have indistinguishable metal content. Outliers that we suggest may need to have their classifications reconsidered are Acfer 202 (CO), Elephant Moraine (EET) 96026 (C4–5), Meteorite Hills (MET) 01149, and Northwest Africa (NWA) 521 (CK), Asuka (A)-88198, LaPaz Icefield (LAP) 031156, and Sahara 98248 (R). χ values can also be used to define affinities of ungrouped chondrites, and propose pairing, particularly in the case of CM and CV meteorites.
  3. ^ Abstract: A database of magnetic susceptibility measurements of stony achondrites (acapulcoite-lodranite clan, winonaites, ureilites, angrites, aubrites, brachinites, howardite-eucrite-diogenite (HED) clan, and Martian meteorites, except lunar meteorites) is presented and compared to our previous work on chondrites. This database provides an exhaustive study of the amount of iron-nickel magnetic phases (essentially metal and more rarely pyrrhotite and titanomagnetite) in these meteorites. Except for ureilites, achondrites appear much more heterogeneous than chondrites in metal content, both at the meteorite scale and at the parent body scale. We propose a model to explain the lack of or inefficient metal segregation in a low gravity context. The relationship between grain density and magnetic susceptibility is discussed. Saturation remanence appears quite weak in most metal-bearing achondrites (HED and aubrites) compared to Martian meteorites. Ureilites are a notable exception and can carry a strong remanence, similar to most chondrites.

Linki zewnętrzne

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