Multidimensional simulations of the accretion-induced collapse of white dwarfs to neutron stars

We present 2.5-dimensional radiation-hydrodynamics simulations of the accretion-induced collapse (AIC) of white dwarfs, starting from two-dimensional rotational equilibrium configurations, thereby accounting consistently for the effects of rotation prior to and after core collapse.We focus our study on a 1.46 and a 1.92M a model. Electron capture leads to the collapse to nuclear densities of these cores a few tens of milliseconds after the start of the simulations. The shock generated at bounce moves slowly, but steadily, outward. 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 40 opening angle about the poles, with a mass loss rate of (5 8) ; 10 3 M s 1. The ejecta have an entropy on the order of (20–50)kB baryon 1 and an electron fraction that is bimodal. By the end of the simulations, at k600 ms after bounce, the explosion energy has reached (3 4) ; 1049 ergs and the mass has reached a few times 10 3M .We estimate the asymptotic explosion energies to be lower than 1050 ergs, 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 ‘‘ ’’ and ¯ e neutrino luminosities are reduced compared to the e neutrino luminosity; the deleptonized region has a butterfly shape; the neutrino flux and electron fraction depends strongly upon latitude (a la von Zeipel ); and a quasi-Keplerian 0.1–0.5 M accretion disk is formed.