Evolution of long-period, white-dwarf binaries: application to GRO J1744-28 and type Ia supernovae

Details Evolution of long-period, white-dwarf binaries: application to GRO J1744-28 and type Ia supernovae Evolution of long-period, white-dwarf binaries: application to GRO J1744-28 and type Ia supernovae

Feb 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009a%26a...495..243x&link_type=abstract

Astronomy and Astrophysics, Volume 495, Issue 1, 2009, pp.243-248

Astronomy and Astrophysics

Astrophysics

14

Accretion, Accretion Disks, Stars: Dwarf Novae, Stars: Pulsars: Individual: Gro J1744-28, Stars: Supernovae: General

Scientific paper

We calculated the evolution of long-period white dwarf binaries, by accounting for thermally unstable accretion during mass transfer. Under certain conditions we found that, the accretion rates onto the white dwarf during dwarf nova outbursts can be sufficiently high to allow steady nuclear burning of the accreted matter and growth of the white dwarf mass. If the Chandrasekhar mass is reached, the white dwarf may collapse to be a neutron star, or explode as a type Ia supernova. This scenario appears to account well for the formation of the bursting pulsar GRO J1744-28, and probably type Ia supernovae with delay times considerably longer than 1 Gyr.

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