The Oxygen to Carbon Ratio in the Solar Interior: Information from Nuclear Reaction Cross-Sections

Abstract

Mass separation in the Sun may explain a serious difficulty that has plagued nuclear astrophysics for decades: Why the oxygen to carbon ratio in the Sun's photosphere is only two, O/C ≈ 2. After correcting for mass fractionation, the ratio of these helium-burning products in the Sun is much larger, O/C ≈ 9-10. The lower value, O/C ≈ 9, is probably more reliable. It is based on measurements of mass separation of stable noble gas isotopes in the solar wind over the mass range of 3-136 amu. The higher value, O/C ≈ 10, is based on a comparison of neutron-capture cross-sections and the abundances of s-products in the photosphere over the mass range of 25-207 amu. Both methods indicate that Fe, Ni, O, Si, and S are the most abundant elements in the Sun. These elements are produced in the deep interior of supernovae.

Department(s)

Chemistry

Sponsor(s)

Foundation for Chemical Research
University of Missouri--Rolla

Keywords and Phrases

Astrophysics; Carbon; Combustion; Fractionation; Helium; Iron; Isotopes; Nickel; Oxygen; Sun; Composition of the Sun; Helium-Burning; S-Products in the Sun; Solar O/C Ratio; Fusion Reactions; Composition of the Sun; Helium-Burning; S-Products in the Sun; Solar O/C Ratio

International Standard Serial Number (ISSN)

0164-0313

Document Type

Article - Journal

Document Version

Citation

File Type

text

Language(s)

English

Rights

© 2004 Springer Verlag, All rights reserved.

Publication Date

01 Mar 2004

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