The binding energy produced within the framework of the accretion of millisecond pulsars

TL;DR

This paper investigates how binding energy during accretion-induced collapse influences millisecond pulsar formation, highlighting the sensitivity to the equation of state and implications for binary system evolution.

Contribution

It introduces a binding energy model for accreting white dwarfs leading to MSPs, emphasizing the role of initial conditions and the equation of state in binary evolution.

Findings

Binding energy affects neutron star mass and gravitational properties.

Accretion-induced collapse can produce low-mass white dwarf companions.

Results constrain neutron star mass and binding energy based on accretion rates.

Abstract

The role and implication of binding energy through the accretion-induced collapse (AIC) of accreting white dwarfs (WDs) for the production of millisecond pulsars (MSPs) are investigated. I examine the binding energy model due to the dynamical process in close binary systems and investigating the possible mass of the companion sufficient to induce their orbital parameters. The deterministic nature of this interaction has a strong sensitivity to the equation of state of the binary systems (where the compactness of a neutron star is proportional to the amount of binding energy) associated with their initial conditions. This behavior will mimic the commonly assumed mass and amount of accreted matter under the instantaneous mass loss ($\Delta M \sim 0.18M_{\odot}$). As a result, this will indicate an increase in the MSP's gravitational mass due to angular momentum losses. The outcome of such a system will then be a circular binary MSP in which the companion is a low-mass WD, thus distinguishing the binary formation scenarios. In addition, the results of this work could provide constraints on the expected mass and binding energy of a neutron star based on the accretion rate