We present 2.5D radiation-hydrodynamics simulations of the accretion-induced collapse ( AIC ) of white dwarfs , starting from 2D rotational equilibrium configurations of a 1.46-M _ { \odot } and a 1.92-M _ { \odot } model .
Electron capture leads to the collapse to nuclear densities of these cores within a few tens of milliseconds .
The shock generated at bounce moves slowly , but steadily , outwards .
Within 50-100 ms , the stalled shock breaks out of the white dwarf along the poles .
The blast is followed by a neutrino-driven wind that develops within the white dwarf , in a cone of \sim 40 ^ { \circ } opening angle about the poles , with a mass loss rate of 5-8 \times 10 ^ { -3 } M _ { \odot } yr ^ { -1 } .
The ejecta have an entropy on the order of 20-50 k _ { B } /baryon , and an electron fraction distribution that is bimodal .
By the end of the simulations , at \geq 600 ms after bounce , the explosion energy has reached 3-4 \times 10 ^ { 49 } erg and the total ejecta mass has reached a few times 0.001 M _ { \odot } .
We estimate the asymptotic explosion energies to be lower than 10 ^ { 50 } erg , significantly lower than those inferred for standard core collapse .
The AIC of white dwarfs thus represents one instance where a neutrino mechanism leads undoubtedly to a successful , albeit weak , explosion .

We document in detail the numerous effects of the fast rotation of the progenitors : The neutron stars are aspherical ; the “ \nu _ { \mu } ” and \bar { \nu } _ { e } neutrino luminosities are reduced compared to the \nu _ { e } neutrino luminosity ; the deleptonized region has a butterfly shape ; the neutrino flux and electron fraction depend strongly upon latitude ( Ã la von Zeipel ) ; and a quasi-Keplerian 0.1-0.5-M _ { \odot } accretion disk is formed .