The binary model for type I supernovae - Theoretical rates

Details The binary model for type I supernovae - Theoretical rates The binary model for type I supernovae - Theoretical rates

Feb 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983a%26a...118..217g&link_type=abstract

Astronomy and Astrophysics, vol. 118, no. 2, Feb. 1983, p. 217-222.

Astronomy and Astrophysics

Astrophysics

266

Astrophysics, Binary Stars, Stellar Models, Supernovae, Elliptical Galaxies, Galactic Radiation, Nuclear Fusion, Rates (Per Time), Ultraviolet Radiation

Scientific paper

Supernovae of type I (or their progenitors) are very likely to play a key role in a variety of astrophysical contexts, including galactic nucleosynthesis, the ultraviolet radiation from stellar populations, and the dynamics of the interstellar medium in galaxies. The knowledge of the rate of type I supernovae is then a crucial requisite for any investigation on these matters. In this paper it is shown that the binary models of type I supernovae naturally account for the occurrence of these events in elliptical galaxies and for their higher rates in late-type galaxies. It is further shown that, if binary models are to account for the observed rates of type I supernovae, then a major fraction of binaries in the appropriate mass ranges must ultimately produce a supernova I event.

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