期刊
ASTROPHYSICAL JOURNAL
卷 591, 期 2, 页码 1220-1247出版社
IOP PUBLISHING LTD
DOI: 10.1086/375492
关键词
astrochemistry; meteors, meteoroids; solar system : formation; Sun : abundances; Sun : photosphere
Solar photospheric and meteoritic CI chondrite abundance determinations for all elements are summarized and the best currently available photospheric abundances are selected. The meteoritic and solar abundances of a few elements ( e. g., noble gases, beryllium, boron, phosphorous, sulfur) are discussed in detail. The photospheric abundances give mass fractions of hydrogen (X = 0.7491), helium (Y = 0.2377), and heavy elements (Z = 0.0133), leading to Z/X = 0.0177, which is lower than the widely used Z/X = 0.0245 from previous compilations. Recent results from standard solar models considering helium and heavy-element settling imply that photospheric abundances and mass fractions are not equal to protosolar abundances ( representative of solar system abundances). Protosolar elemental and isotopic abundances are derived from photospheric abundances by considering settling effects. Derived protosolar mass fractions are X-0 = 0.7110, Y-0 = 0.2741, and Z(0) = 0.0149. The solar system and photospheric abundance tables are used to compute self-consistent sets of condensation temperatures for all elements.
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