Evolution of Fe, r, and S elements in our Galaxy

Details Evolution of Fe, r, and S elements in our Galaxy Evolution of Fe, r, and S elements in our Galaxy

Nov 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...334..698a&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 334, Nov. 15, 1988, p. 698-706. CNRS-supported research.

Astronomy and Astrophysics

Astrophysics

19

Chemical Evolution, Galactic Evolution, Milky Way Galaxy, Nuclear Astrophysics, Star Formation Rate, Hubble Constant, Iron, Neodymium, Nuclear Fusion, Stellar Composition, Thorium

Scientific paper

Constraints are set up here on the first generations of disk stars by taking advantage of the sensitivity of Fe, r, and s abundances against the star formation rate for stars of different masses. A time-varying SFR and a bimodal SFR which differ in their predicted proportion of massive stars at early epochs are considered. The analysis reported here clearly favors time-varying SFR models which account satisfactorily for both the r and s abundance similarity in the solar system and the overall metallicity such as the sharp rise of the r-process nuclei relative to the s-process nuclei. The evolution of the Th/Nd ratio is also considered.

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