  It has been suggested that the accretion-induced collapse (AIC) of an
oxygen-neon white dwarf (ONe WD) to a neutron star is a theoretically predicted
outcome in stellar evolution, likely relating to the formation of some neutron
star systems. However, the progenitor models of AIC events are still not well
studied, and recent studies indicated that CO WD+He star systems may also
contribute to the formation of neutron star systems through AIC process when
off-centre carbon ignition happens on the surface of the CO WD. In this work, I
studied the single-degenerate (SD) model of AIC events in a systematic way,
including the contribution of the CO WD+He star channel and the ONe WD+MS/RG/He
star channels. Firstly, I gave the initial parameter space of these SD channels
for producing AIC events in the orbital period--secondary mass plane based on
detailed binary evolution computations. Then, according to a binary population
synthesis approach, I gave the rates and delay times of AIC events for these SD
channels based on their initial parameter space. I found that the rates of AIC
events in our galaxy are in the range of
$\sim0.3-0.9\times10^{-3}$\,yr$^{-1}$,and that their delay times are
$>$30\,Myr. I also found that the ONe WD+He star channel is the main way to
produce AIC events, and that the CO WD+He star channel cannot be ignored when
studying the progenitors of AIC events.
