  Accretion-induced collapse of massive white dwarfs (WDs) has been proposed to
be an important channel to form binary millisecond pulsars (MSPs). Recent
investigations on thermal timescale mass transfer in WD binaries demonstrate
that the resultant MSPs are likely to have relatively wide orbit periods
($\gtrsim 10$ days). Here we calculate the evolution of WD binaries taking into
account the excited wind from the companion star induced by X-ray irradiation
of the accreting WD, which may drive rapid mass transfer even when the
companion star is less massive than the WD. This scenario can naturally explain
the formation of the strong-field neutron star in the low-mass X-ray binary 4U
1822$-$37. After AIC the mass transfer resumes when the companion star refills
its Roche lobe, and the neutron star is recycled due to mass accretion. A large
fraction of the binaries will evolve to become binary MSPs with a He WD
companion, with the orbital periods distributed between $\gtrsim 0.1$ day and
$\lesssim 30$ days, while some of them may follow the cataclysmic variable-like
evolution towards very short orbits. If we instead assume that the newborn
neutron star appears as an MSP and part of its rotational energy is used to
ablate its companion star, the binaries may also evolve to be the redback-like
systems.

High Energy Astrophysical Phenomena