  Recently observed pulsars with masses $\sim 1.1 ~M_{\odot}$ challenge the
conventional neutron star (NS) formation path by core-collapse supernova
(CCSN). Using spherically symmetric hydrodynamics simulations, we follow the
collapse of a massive white dwarf (WD) core triggered by electron capture,
until the formation of a proto-NS (PNS). For initial WD models with the same
central density, we study the effects of a static, compact dark matter (DM)
admixed core on the collapse and bounce dynamics and mass of the PNS, with DM
mass $\sim 0.01 ~M_{\odot}$. We show that increasing the admixed DM mass
generally leads to slower collapse and smaller PNS mass, down to about 1.0
$M_{\odot}$. Our results suggest that the accretion-induced collapse of dark
matter admixed white dwarfs can produce low-mass neutron stars, such as the
observed low-mass pulsar J0453+1559, which cannot be obtained by conventional
NS formation path by CCSN.

High Energy Astrophysical Phenomena;Solar and Stellar Astrophysics