  We present axisymmetric hydrodynamical simulations of accretion-induced
collapse (AIC) of dark matter (DM) admixed rotating white dwarfs (WD) and their
burst gravitational-wave (GW) signals. For initial WD models with the same
central baryon density, the admixed DM is found to delay the plunge and bounce
phases of AIC, and decrease the central density and mass of the proto-neutron
star (PNS) produced. The bounce time, central density and PNS mass generally
depend on two parameters, the admixed DM mass $M_\mathrm{DM}$ and the ratio
between the rotational kinetic and gravitational energies of the inner core at
bounce $\beta_\mathrm{ic,b}$. The emitted GWs have generic waveform shapes and
the variation of their amplitudes $h_+$ show a degeneracy on
$\beta_\mathrm{ic,b}$ and $M_\mathrm{DM}$. We found that the ratios between the
GW amplitude peaks around bounce allow breaking the degeneracy and extraction
of both $\beta_\mathrm{ic,b}$ and $M_\mathrm{DM}$. Even within the
uncertainties of nuclear matter equation of state, a DM core can be inferred if
its mass is greater than 0.03 $M_{\odot}$. We also discuss possible DM effects
on the GW signals emitted by PNS g-mode oscillations. GW may boost the
possibility for the detection of AIC, as well as open a new window in the
indirect detection of DM.
