Abia, C.; Canal, R.; Isern, J.
Bibliographical reference
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 366, Jan. 1, 1991, p. 198-202. Research supported by CICYT.
Advertised on:
1
1991
Journal
Citations
23
Refereed citations
22
Description
The new observational O/Fe versus Fe/H abundance relationship for halo
stars is studied in terms of several models of chemical evolution for
the solar neighborhood. Nucleosynthesis products from type I (both Ia
and Ib) and Type II SNs are taken into account. The behavior of the O/Fe
ratio for halo and disk stars is well reproduced by assuming (1) a lower
iron production in SN II than in previous theoretical prescriptions, (2)
the coalescence by gravitational wave radiation of two CO white dwarfs
as the scenario for type Ia supernovae, and (3) stars in the Wolf-Rayet
stage as progenitors of type Ib supernovae. Nevertheless, the best
agreement with the observations is obtained by adopting an IMF favoring
massive star formation only at very early epochs in the life of the
Galaxy. Model predictions from other plausible scenarios for the origin
of type I supernovae are also discussed.