Astronomy and Astrophysics – Astrophysics
Scientific paper
Apr 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...315..229k&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 315, April 1, 1987, p. 229-233.
Astronomy and Astrophysics
Astrophysics
45
Eclipsing Binary Stars, Nuclear Astrophysics, Nuclear Fusion, Stellar Interiors, Stellar Mass Accretion, White Dwarf Stars, Carbon, Helium, Stellar Composition, Stellar Evolution, Stellar Mass, Symmetry
Scientific paper
The ignition of nuclear burning in merging white dwarfs is investigated for various combinations of component stars composed of He, C + O, and O + Ne + Mg. It is assumed that a rapidly accreting white dwarf mimics the massive component of a merging double-white-dwarf binary system. By computing steady models the location of nuclear ignition is obtained as a function of the accretion rate and the mass of accreting stars. For C + O dwarf pairs, accretion at a rate higher than about 2.7 x 10 to the -6th solar mass/yr leads to the off-center carbon ignition. The white dwarf mass (WDM) at the off-center ignition is smaller for higher accretion rate. For the highest accretion rate, the Eddington accretion limit, WDM = 1.07 solar mass when carbon ignites off-center. For WDM smaller than this value, no carbon ignition occurs. The off-center Ne ignition in an O + Ne + Mg white dwarf does not occur even in a model with the Eddington accretion rate. Helium ignition in He-accreting C + O white dwarfs is also considered.
Kawai Yasushi
Nomoto Ken'ichi
Saio Hideyuki
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