Oxygen Isotopic Measurements of Calcite Grains in a Refractory Inclusion by Nano-SIMS: Implications to The Formation Process of Carbonate in the Early Solar Nebula

Details Oxygen Isotopic Measurements of Calcite Grains in a Refractory Inclusion by Nano-SIMS: Implications to The Formation Process of Carbonate in the Early Solar Nebula Oxygen Isotopic Measurements of Calcite Grains in a Refractory Inclusion by Nano-SIMS: Implications to The Formation Process of Carbonate in the Early Solar Nebula

Dec 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmmr13b1711k&link_type=abstract

American Geophysical Union, Fall Meeting 2008, abstract #MR13B-1711

Other

1028 Composition Of Meteorites (3662, 6240), 3662 Meteorite Mineralogy And Petrology (1028, 6240), 6210 Comets (6023), 6213 Dust, 6240 Meteorites And Tektites (1028, 3662)

Scientific paper

Refractory inclusions (CAIs) from chondritic meteorites are widely considered to represent the first materials that formed in the solar nebula (MacPherson et al. 1988). We discovered for the first time a unique spherical CAI, which consist of calcite, spinel, diopside and PCP from Murchison meteorite. Inside of this refractory inclusion, calcite, spinel, diopside coexist each other and include abundant vacancies. Calcite is always surrounded by diopside and spinel. Direct evidence for in situ formation of the secondary phases, such as veins, is totally absent. Replacement is not also recognized. The oxygen isotopic data are plotted into two distinct regions on three isotopic diagram. The primary phases of spinel and diopside have typical 16O-enriched values of -40 to -50 , while calcite are plotted 16O-riched values of -5 to -20 on the CCAM line. The degree of 16O-enrichiment of spinel and diopside is similar to those in non-altered CAIs of CV chondrites. The 16O-riched values of calcite do not support the model such as alteration products in the meteorite parent body after CAI solidification. Our result indicates that calcite formed initially 16O-rich region similar to most of refractory objects. Therefore, We think that the calcite in this refractory inclusion should be already formed in the early solar nebula. In fact, carbonate is usually attributed to aqueous alteration in solar system objects (on Earth or in meteorites). A recent study suggests that carbonate may form in the presence of water vapor in solar type proto-stars (Ceccarelli et al. 2002). The detection of calcite in solar type proto-stars, where no liquid water has existed, represents a new frontier in carbonate formation theories. The textual occurrences and isotopic evidence of calcite in this refractory inclusion are clearly compatible with such a report.

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