Existence of an 16 O-Rich Gaseous Reservoir in the Solar Nebula-Reference-Cited by-同舟云学术

Existence of an 16 O-Rich Gaseous Reservoir in the Solar Nebula

Published:2002-02-08 Issue:5557 Volume:295 Page:1051-1054
ISSN:0036-8075
Container-title:Science
language:en
Short-container-title:Science

Author:

Krot Alexander N.¹,McKeegan Kevin D.²,Leshin Laurie A.³,MacPherson Glenn J.⁴,Scott Edward R. D.¹

Affiliation:

1. Hawaii Institute of Geophysics and Planetology, School of Ocean and Earth Science and Technology, University of Hawaii, Honolulu, HI 96822, USA.

2. Department of Earth and Space Sciences, University of California, Los Angeles, Los Angeles, CA 90095–1567, USA.

3. Department of Geological Sciences, Arizona State University, Tempe, AZ 85287–1404, USA.

4. Department of Mineral Sciences, U.S. National Museum of Natural History, Smithsonian Institution, Washington, DC 20560–0119, USA.

Abstract

Carbonaceous chondrite condensate olivine grains from two distinct petrographic settings, calcium-aluminum–rich inclusion (CAI) accretionary rims and amoeboid olivine aggregates (AOAs), are oxygen-16 ( 16 O) enriched at the level previously observed inside CAIs. This requires that the gas in the nebular region where these grains condensed was 16 O-rich. This contrasts with an 16 O-poor gas present during the formation of chondrules, suggesting that CAIs and AOAs formed in a spatially restricted region of the solar nebula containing 16 O-rich gas. The 16 O-rich gas composition may have resulted either from mass-independent isotopic chemistry or from evaporation of regions with enhanced dust/gas ratios, possibly in an X-wind environment near the young Sun.

Publisher

American Association for the Advancement of Science (AAAS)

Subject

Multidisciplinary

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