Formation of ureilites by nebular processes

Details Formation of ureilites by nebular processes Formation of ureilites by nebular processes

May 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988gecoa..52.1313c&link_type=abstract

Geochimica et Cosmochimica Acta (ISSN 0016-7037), vol. 52, May 1988, p. 1313-1318.

Other

63

Meteorites, Meteoritic Composition, Ureilites, Fractionation, Nebulae, Oxygen Isotopes, Meteorites, Ureilites, Formation, Origin, Oxygen, Isotopes, Procedure, Samples, Meteorite, Laboratory Studies, Antarctic Meteorites, Chemistry, Solar Nebula, Parent Bodies, Catalog

Scientific paper

Oxygen isotopic data are presented for 23 ureilites, including 14 Antarctic meteorites. They show a much greater range in isotopic composition than those previously studied. Most noteworthy is the fact that, unlike other achondrite groups, the ureilites do not fall on a mass-dependent isotopic fractionation trend, but rather fall along an extrapolation of the O-16 mixing line defined by components of Allende and other C3 chondrites. Correlations between isotopic and chemical data imply that the isotopic and chemical variations are due primarily to processes in the solar nebula and not to igneous processes within a parent body. The ureilite parent body accreted with isotopic and chemical heterogeneities which were not much modified by subsequent parent-body processes. The precursor materials were related in some way to the C3 carbonaceous chondrites.

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