# Towards an accurate description of an accretion induced collapse and the associated ejected mass

## TL;DR

This paper models the accretion-induced collapse of white dwarfs into neutron stars, focusing on accurately simulating the ejected mass and its potential observational signatures, with implications for fast radio bursts and optical transients.

## Contribution

It provides detailed hydrodynamic simulations of AIC with improved treatment of the equation of state and nuclear burning, estimating ejected mass across various parameters.

## Key findings

- Ejected mass ranges from 0.01 to 0.1 solar masses.
- Simulation results are explained by a simple theoretical model.
- Focus on accurate hydrodynamics without neutrino or GR effects.

## Abstract

We revisit the accretion-induced collapse (AIC) process, in which a white dwarf collapses into a neutron star. We are motivated by the persistent radio source associated with the fast radio burst FRB 121102, which was explained by Waxman as a weak stellar explosion with a small ($\sim 10^{-5}M_{\odot}$) mildly relativistic mass ejection that may be consistent with AIC. Additionally, the interaction of the relatively low ejected mass with a pre-collapse wind might be related to fast optical transients. The AIC is simulated with a one-dimensional, Lagrangian, Newtonian hydrodynamic code. We put an emphasis on accurately treating the equation of state and the nuclear burning, which is required for any study that attempts to accurately simulate AIC. We leave subjects such as neutrino physics and general relativity corrections for future work. Using an existing initial profile and our own initial profiles, we find that the ejected mass is $\sim 10^{-2}$ to $10^{-1}M_{\odot}$ over a wide range of parameters, and we construct a simple model to explain our results.