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Supernovae of type I as end products of the evolution of binaries with components of moderate initial mass (M not greater than about 9 solar masses)
Iben, I., Jr.; Tutukov, A. V.
AA(Illinois, University, Urbana, IL)
Astrophysical Journal Supplement Series (ISSN 0067-0049), vol. 54, Feb. 1984, p. 335-372. (ApJS Homepage)
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NASA/STI Keywords:
Binary Stars, Stellar Evolution, Stellar Mass, Supernovae, Dwarf Stars, Planetary Nebulae, Red Giant Stars, Stellar Cores, Stellar Envelopes, Stellar Mass Accretion, Stellar Winds, X Ray Sources
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Formation frequencies of binary systems which may become Type I supernovae are estimated. Presupernova systems consist of a CO or He degenerate dwarf and a (potential) mass donor (main-sequence star = MS; low-mass red giant = RG; asymptotic giant branch star = AGB; CO or He degenerate dwarf = CODD or HeDD). Mass transfer is driven by nuclear evolution (E), capture from wind (W), a magnetic stellar wind (MSW), or gravitational wave radiation (GWR). For several scenarios, the composition of accretor, nature of donor, driving mechanism, and formation frequency (in 10-3 yr-1 per 1010 L_sun; in the B band), respectively, are the following: (1) CO, RG, E, 10-2- 10-3; (2) CO, AGB, W, 4; (3) CO, MS, MSW, 2; (4) He, MS, MSW, 2; (5) CO or He, near-MS, E+MSW, 3; (6) CO, CODD, GWR, 8; (7) CO, HeDD, GWR, 1; (8) He, HeDD, GWR, 5. The galactic Type I supernova frequency is 10.

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