Astronomy and Astrophysics – Astrophysics
Scientific paper
Oct 1978
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978apj...225..212w&link_type=abstract
Astrophysical Journal, Part 1, vol. 225, Oct. 1, 1978, p. 212-220.
Astronomy and Astrophysics
Astrophysics
51
Carbon Stars, Crab Nebula, R Coronae Borealis Stars, Supergiant Stars, Supernovae, Variable Stars, Abundance, Elliptical Galaxies, Red Giant Stars, Stellar Evolution, Stellar Mass
Scientific paper
Present observations and theory point to Type I supernovae (SN I) as being old disk-population helium-rich red supergiants at the time of outburst. There is a class of stars which correspond to these specifications, the hydrogen-deficient carbon (Hd C) stars, the best known subclass of which are the R Coronae Borealis variables; hence these stars may be SN I progenitors. Within present rather large uncertainties the rate of production of Hd C stars is consistent with the rate of Type I supernovae in the Galaxy. Paczynski's (1971) suggestion that R Coronae Borealis stars are mixed, completely hydrogen-depleted stars of 1-2 solar masses may call for extended main-sequence lifetimes, which in turn would explain how stars with masses greater than the Chandrasekhar mass are only now evolving to explosive end points in elliptical galaxies. The Crab Nebula, being helium-rich, metal-poor, and apparently of only moderate mass, may also be related to this class of event.
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