Evolution of post-Accretion Induced Collapse Binaries: the Effect of Evaporation

TL;DR

This paper investigates how evaporation affects the evolution of post-accretion-induced collapse binaries, potentially explaining observed redback and black widow pulsar systems.

Contribution

It introduces a detailed model of binary evolution considering evaporation effects before and during Roche-lobe overflow, highlighting the influence of key parameters.

Findings

Evaporation significantly alters binary evolution pathways.

The model can reproduce observed redback and black widow systems.

Parameter variations impact the final companion mass and orbital period.

Abstract

Accretion-induced collapse (AIC) is widely accepted to be one of the formation channels for millisecond pulsars (MSPs). Since the MSPs have high spindown luminosities, they can immediately start to evaporate their companion stars after birth. In this paper we present a detailed investigation on the evolution of the post-AIC binaries, taking into account the effect of evaporation both before and during the Roche-lobe overflow process. We discuss the possible influence of the input parameters including the evaporation efficiency, the initial spin period and the initial surface magnetic field of the newborn neutron star. We compare the calculated results with the traditional low-mass X-ray binary evolution, and suggest that they may reproduce at least part of the observed redbacks and black widows in the companion mass - orbital period plane depending on the mechanisms of angular momentum loss associated with evaporation.