On the formation of neutron stars via accretion-induced collapse in binaries

Understand

We investigate evolutionary pathways leading to neutron star formation through the collapse of oxygen-neon white dwarf (ONe WD) stars in interacting binaries.

• We consider (1) non-dynamical mass transfer where an ONe WD approaches the Chandrasekhar mass leading to accretion-induced collapse (AIC) and (2) dynamical timescale merger-induced collapse (MIC) between an ONe WD and another WD.
• We present rates, delay times, and progenitor properties for two different treatments of common envelope evolution.
• We show that AIC neutron stars are formed via many different channels and the most dominant channel depends on the adopted common envelope physics.