1998A&A...338..957V

We show that all supersoft X-ray binaries should excite strong winds ({dot}(M)_wind∼10^–7M_☉/yr) 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 (M₂/M₁≲0.7), such as the 4hr 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.