Rai, V. K. (2005) Photochemical Mass-Independent Sulfur Isotopes in Achondritic Meteorites. Science, 309 (5737). 1062-1065 doi:10.1126/science.1112954
Reference Type | Journal (article/letter/editorial) | ||
---|---|---|---|
Title | Photochemical Mass-Independent Sulfur Isotopes in Achondritic Meteorites | ||
Journal | Science | ||
Authors | Rai, V. K. | Author | |
Year | 2005 (August 12) | Volume | 309 |
Page(s) | 1062-1065 | Issue | 5737 |
Publisher | American Association for the Advancement of Science (AAAS) | ||
DOI | doi:10.1126/science.1112954Search in ResearchGate | ||
Mindat Ref. ID | 2576752 | Long-form Identifier | mindat:1:5:2576752:8 |
GUID | 6a1d04f9-a624-4a77-a25c-ee72e618dffc | ||
Full Reference | Rai, V. K. (2005) Photochemical Mass-Independent Sulfur Isotopes in Achondritic Meteorites. Science, 309 (5737). 1062-1065 doi:10.1126/science.1112954 | ||
Plain Text | Rai, V. K. (2005) Photochemical Mass-Independent Sulfur Isotopes in Achondritic Meteorites. Science, 309 (5737). 1062-1065 doi:10.1126/science.1112954 | ||
In | (2005, August) Science Vol. 309 (5737) American Association for the Advancement of Science (AAAS) |
References Listed
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There have been numerous presolar oxide grains with anomalous oxygen identified but their abundance is far too small and of the wrong isotopic composition to account for oxygen isotopic anomalies known to be present at the bulk meteorite level [( 2 ) and references therein]. | |
Not Yet Imported: Accounts of Chemical Research - journal-article : 10.1021/ar960224f If you would like this item imported into the Digital Library, please contact us quoting Journal ID 470 | |
M. H. Thiemens, in Treaties on Geochemistry, R. F. Keeling, Ed. (Elsevier, Oxford, 2003), vol. 4, pp. 159–175. | |
Sulfide extractions were done by using the procedure described in ( 13 ); also see online Materials and Methods for more details. The typical errors of δ 33 S δ 34 S and δ 36 S measurements are 0.010 0.010 and 0.200 (in ‰) respectively. | |
We calculated 33 S and 36 S enrichment with the following equation: Δ 33 S = δ 33 S – 1000[(1 + δ 34 S/1000) 0.515 – 1] and Δ 36 S = δ 36 S – 1000[(1 + δ 34 S/1000) 1.91 – 1]. | |
Y. N. Chin, C. Henkel, J. B. Whiteoak, N. Langer, E. B. Churchwell, Astron. Astrophys.305, 960 (1996). | |
As a result of its small abundance δ 36 S is sensitive to contaminations at any stage from chemical extraction or gas chromatography or during measurements. The reported error on δ 36 S is only measurement error; the actual uncertainty due to contamination might be higher. | |
A. N. Krot, B. Fegley, K. Lodders, H. Palme, in Protostars and Planets IV, V. Mannings, A. P. Boss, S. S. Russell, Eds. (Univ. of Arizona, Tucson, AZ, 2000), pp. 1019–1054. | |
NASA Cosmochemistry program is gratefully acknowledged for support of this research. |
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