Helium star cataclysmics

Journal Article · Mon Apr 01 04:00:00 EST 1991 · Astrophysical Journal; (USA)

DOI:https://doi.org/10.1086/169848· OSTI ID:5759882

Tutukov, A V ^[1]

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1. Pennsylvania State Univ., University Park (USA) Astronomicheskii Sovet, Moscow (USSR)

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. 65 refs.

• OSTI ID: 5759882
• Journal Information: Astrophysical Journal; (USA), Journal Name: Astrophysical Journal; (USA) Vol. 370; ISSN ASJOA; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

640102* -- Astrophysics & Cosmology-- Stars & Quasi-Stellar
Radio & X-Ray Sources
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
BINARY STARS
DWARF STARS
ELEMENTS
ERUPTIVE VARIABLE STARS
FLUIDS
GASES
HELIUM
HELIUM BURNING
MASS
MASS TRANSFER
NEBULAE
NONMETALS
NOVAE
NUCLEOSYNTHESIS
PLANETARY NEBULAE
RARE GASES
STAR ACCRETION
STAR BURNING
STAR EVOLUTION
STARS
SUPERNOVAE
SYNTHESIS
VARIABLE STARS
WHITE DWARF STARS