Astronomy and Astrophysics – Astrophysics
Scientific paper
Apr 1991
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apj...370..615i&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 370, April 1, 1991, p. 615-629. Pennsylvania State University-supported res
Astronomy and Astrophysics
Astrophysics
95
Binary Stars, Dwarf Novae, Helium, Stellar Evolution, Stellar Interiors, Supernovae, White Dwarf Stars, Mass Transfer, Nuclear Fusion, Stellar Mass Accretion, Stellar Temperature
Scientific paper
Scenarios for the formation of systems in which a carbon-oxygen white dwarf accretes helium from a nondegenerate companion that burns helium in its core are considered. The mass transfer rate in such systems is about 300 times larger than that anticipated for classical hydrogen-transferring cataclysmic variables with orbital periods less than two hours, and the lifetime is some 200 times smaller than that of short-period classical cataclysmics. After the transfer of about 0.15 solar mass of helium onto a dwarf of initial mass 0.6-1 solar, a thermonuclear runaway occurs in the accreted layer. If the mass of the accretor is about 0.6 solar, the system may appear as a short-lived helium PN. If it remains visible for about 100 yr, there may be one such supernova at any time in the Galaxy at a luminosity of the order 10,000 solar. If the mass of the accretor is 1 solar or larger, an explosion of weak supernova magnitude will occur. Perhaps two in 10 supernovae may be of this variety.
Iben Icko Jr.
Tutukov Alexander V.
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