Double white dwarfs as progenitors of R Coronae Borealis stars and Type I supernovae

Details Double white dwarfs as progenitors of R Coronae Borealis stars and Type I supernovae Double white dwarfs as progenitors of R Coronae Borealis stars and Type I supernovae

Feb 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...277..355w&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 277, Feb. 1, 1984, p. 355-360.

Astronomy and Astrophysics

Astrophysics

763

Binary Stars, Corona Borealis Constellation, R Coronae Borealis Stars, Stellar Evolution, Supernovae, White Dwarf Stars, B Stars, Carbon Stars, Chandrasekhar Equation, O Stars, Stellar Mass Accretion, Stellar Mass Ejection

Scientific paper

Tidal mass transfer in double degenerate systems is explored. The sequence of double white dwarfs divides naturally into three segments: (1) low-mass helium/helium pairs are unstable to dynamical time-scale mass transfer and probably coalesce to form helium-burning sdO stars; (2) in helium/carbon-oxygen pairs, mass transfer occurs on the time scale for gravitational radiation losses; the accreted helium is quickly ignited, and the accretor expands to dimensions characteristic of R CrB stars, engulfing its companion star; and (3) carbon-oxygen/carbon-oxygen pairs are again unstable to dynamical time-scale mass transfer and, since their total masses exceed the Chandrasekhar limit, are destined to become supernovae. Inactive lifetimes in these latter systems between creation and interaction can exceed 10 billion years. Birthrates of R CrB stars and Type I supernovae by evolution of double white dwarfs are in reasonable agreement with observational estimates.

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