Wind-driven evolution of supersoft X-ray binaries with low-mass secondaries

Details Wind-driven evolution of supersoft X-ray binaries with low-mass secondaries Wind-driven evolution of supersoft X-ray binaries with low-mass secondaries

Oct 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998a%26a...338..957v&link_type=abstract

Astronomy and Astrophysics, v.338, p.957-964 (1998)

Astronomy and Astrophysics

Astrophysics

39

Accretion, Accretion Disks, Stars: Individual: 1E 0035.4-7230, Stars: Mass-Loss, Novae, Cataclysmic Variables, Supernovae: General, X-Rays: Stars

Scientific paper

We show that all supersoft X-ray binaries should excite strong winds (Mdot_wind \sim 10^{-7} M_{\sun} yr^{-1}) from the irradiated companion star. Scattering and absorption in this wind is likely to have a significant effect on the orbital X-ray light curve. In systems with a low-mass companion (M_2/M_1 \la 0.7$), such as the 4 hr supersoft X-ray binary 1E 0035.4-7230, the angular momentum loss in the wind may dominate the binary evolution and drive Roche lobe overflow at a rate comparable to the wind-loss rate. This may self-consistently sustain stable recurrent or steady-state hydrogen burning on the accreting white dwarf and keep the binary as a supersoft X-ray binary. These low-mass wind-driven supersoft X-ray binaries evolve towards longer periods, and can cross the period region populated by supersoft X-ray binaries driven by thermal-timescale mass transfer from a companion star more massive than the white dwarf. Starting from a massive white dwarf, low-mass wind-driven supersoft X-ray binaries may drive the white dwarf over the Chandrasekhar limit and produce a type Ia supernova.

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