Binding energy produced within the framework of the accretion of millisecond pulsars

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 investigate the possible mass 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 (M í 0:18Mæ). As a result, this will indicate an increase in the MSP’s gravitational mass due to the 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. I have shown that it is possible to add some constraints on the expected values of the mass and binding energy of a neutron star depending on the accretion rate.