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Cited by 363

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Mineralogy of meteorite groups

RUBIN, Alan E.·1997·Meteoritics & Planetary Science
DOI 10.1111/j.1945-5100.1997.tb01262.x
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Abstract

Abstract— Approximately 275 mineral species have been identified in meteorites, reflecting diverse redox environments, and, in some cases, unusual nebular formation conditions. Anhydrous ordinary, carbonaceous and R chondrites contain major olivine, pyroxene and plagioclase; major opaque phases include metallic Fe‐Ni, troilite and chromite. Primitive achondrites are mineralogically similar. The highly reduced enstatite chondrites and achondrites contain major enstatite, plagioclase, free silica and kamacite as well as nitrides, a silicide and Ca‐, Mg‐, Mn‐, Na‐, Cr‐, K‐ and Ti‐rich sulfides. Aqueously altered carbonaceous chondrites contain major amounts of hydrous phyllosilicates, complex organic compounds, magnetite, various sulfates and sulfides, and carbonates. In addition to kamacite and taenite, iron meteorites contain carbides, elemental C, nitrides, phosphates, phosphides, chromite and sulfides. Silicate inclusions in IAB/IIICD and IIE iron meteorites consist of mafic silicates, plagioclase and various sulfides, oxides and phosphates. Eucrites, howardites and diogenites have basaltic to orthopyroxenitic compositions and consist of major pyroxene and calcic plagioclase and several accessory oxides. Ureilites are made up mainly of calcic, chromian olivine and low‐Ca clinopyroxene embedded in a carbonaceous matrix; accessory phases include the C polymorphs graphite, diamond, lonsdaleite and chaoite as well as metallic Fe‐Ni, troilite and halides. Angrites are achondrites rich in fassaitic pyroxene (i.e., Al‐Ti diopside); minor olivine with included magnesian kirschsteinite is also present. Martian meteorites comprise basalts, lherzolites, a dunite and an orthopyroxenite. Major phases include various pyroxenes and olivine; minor to accessory phases include various sulfides, magnetite, chromite and Ca‐phosphates. Lunar meteorites comprise mare basalts with major augite and calcic plagioclase and anorthositic breccias with major calcic plagioclase. Several meteoritic phases were formed by shock metamorphism. Martensite (α 2‐Fe,Ni) has a distorted body‐centered‐cubic structure and formed by a shear transformation from taenite during shock reheating and rapid cooling. The C polymorphs diamond, lonsdaleite and chaoite formed by shock from graphite. Suessite formed in the North Haig ureilite by reduction of Fe and Si (possibly from olivine) via reaction with carbonaceous matrix material. Ringwoodite, the spinel form of (Mg,Fe)2 SiO 4, and majorite, a polymorph of (Mg,Fe)SiO 3 with the garnet structure, formed inside shock veins in highly shocked ordinary chondrites. Secondary minerals in meteorite finds that formed during terrestrial weathering include oxides and hydroxides formed directly from metallic Fe‐Ni by oxidation, phosphates formed by the alteration of schreibersite, and sulfates formed by alteration of troilite.

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Metadata

Authors
RUBIN, A. E.
Venue
Meteoritics & Planetary Science
Publisher
Wiley
Published
1997-03
Volume
32
Issue
2
Pages
231-247
ISSN
  • 1086-9379 (ISSN-L)
  • 1945-5100
DOI
10.1111/j.1945-5100.1997.tb01262.x
OpenAlex
W2027296098
Cited by
363
References
3
FWCI
3.62
Type
journal article
Language
en
Open access
closed
Licence
onlinelibrary.wiley.com/termsAndConditions#vor (vor, 4723 d)

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