Relative abundances in metal-poor stars. III - Sodium through copper

Details Relative abundances in metal-poor stars. III - Sodium through copper Relative abundances in metal-poor stars. III - Sodium through copper

Mar 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981apj...244..989p&link_type=abstract

Astrophysical Journal, Part 1, vol. 244, Mar. 15, 1981, p. 989-1000.

Other

117

Abundance, Dwarf Stars, Metallic Stars, Stellar Spectra, Subgiant Stars, Aluminum, Copper, Error Analysis, Extraterrestrial Radiation, Hydrogen, Iron, Magnesium, Nuclear Fusion, Sodium, Stellar Atmospheres, Stellar Evolution, Stellar Spectrophotometry, Vanadium

Scientific paper

Patterns of the relative abundances of 15 elements from sodium through the iron peak are identified from self-consistent analyses of more than 30 metal-poor field dwarfs and subgiants. The iron-peak elements are always found in the same proportion as in the sun, while the lighter even-Z elements - magnesium, silicon, calcium, and titanium - appear slightly enhanced. Only aluminum shows instances of large deviations from the solar proportion; for all other elements, except perhaps sodium and magnesium, there is no intrinsic scatter to within about + or - 0.1 dex. Although exceptions do occur, sodium and aluminum both tend to become less and less abundant with respect to iron as the overall level of stellar metallicity diminishes. Explosive nucleosynthesis, which alone has predicted such a trend, is strongly supported by that trend as the mechanism which has produced the heavy elements in these stars. This interpretation demands a connection between the metallicity of the explosive object and that of the subsequent stellar generation. Implications are also noted for the interpretation of extragalactic spectra.

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