  Accretion-induced collapse (AIC) is widely accepted to be one of the
formation channels for millisecond pulsars (MSPs). Since the MSPs have high
spindown luminosities, they can immediately start to evaporate their companion
stars after birth. In this paper we present a detailed investigation on the
evolution of the post-AIC binaries, taking into account the effect of
evaporation both before and during the Roche-lobe overflow process. We discuss
the possible influence of the input parameters including the evaporation
efficiency, the initial spin period and the initial surface magnetic field of
the newborn neutron star. We compare the calculated results with the
traditional low-mass X-ray binary evolution, and suggest that they may
reproduce at least part of the observed redbacks and black widows in the
companion mass - orbital period plane depending on the mechanisms of angular
momentum loss associated with evaporation.
