Wind-driven evolution of accreting binaries and the progenitors of SNe IA

Details Wind-driven evolution of accreting binaries and the progenitors of SNe IA Wind-driven evolution of accreting binaries and the progenitors of SNe IA

Oct 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998a%26a...338..965k&link_type=abstract

Astronomy and Astrophysics, v.338, p.965-970 (1998)

Astronomy and Astrophysics

Astrophysics

11

Accretion, Accretion Disks, Stars: Mass-Loss, Novae, Cataclysmic Variables, Supernovae: General, White Dwarfs, X-Rays: Stars

Scientific paper

Strong self-excited winds from the companion are very likely in many accreting binaries, and we investigate their evolutionary effects. We show that in white dwarf systems with large mass ratios M_2/M_1 ga 1.3, self-excited winds naturally stabilize mass transfer at a threshold value {M}_b ~ 10(-8}M_{sun ) yr(-1) . Near this threshold value, irradiation-induced wind loss rates from the companion star become much higher, because of intermittent stable hydrogen shell burning on the accreting white dwarf. The white dwarf can accrete a substantial mass ( ~ 0.5M_&sun;) during this evolution, and may produce a Type Ia supernova directly in some cases. In other cases the evolution may produce supersoft X-ray binaries with quite massive white dwarfs and moderate-mass companions, which then undergo thermal-timescale mass transfer and may produce SNe Ia themselves. We show that the stability of such `bootstrap' evolution via a self-excited wind is indeterminate if the wind losses depend linearly on the mass transfer rate, as assumed in some analyses of low-mass X-ray binary evolution. Such analyses must be repeated with a more precise form of the wind-driving law. In practice systems with small mass ratios will tend to stabilize in regimes where the wind-driving law is slower than linear, with the opposite result for large mass ratios.

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