The role of binding energies of neutron stars on the accretion driven evolution

Abstract

Millisecond pulsars are believed to descend from low mass x-ray binaries. Observable parameters of binary millisecond pulsars e.g. mass of the pulsar, mass of the companion, spin period of the pulsar, orbital period, orbital eccentricity etc are used to probe the past accretion history of the millisecond pulsars. But unfortunately in these studies, binding energy of the neutron star is not considered commonly. We show that the effect of the binding energy is significant in the estimation of the amount of mass accretion and thus should be incorporated in models for binary evolutions. Moreover, different Equations of State for dense matter give different values for the accreted mass for the same amount of increase in the gravitational mass of the neutron star implying the need of constraining dense matter Equations of State even to understand the spin-up procedure properly.

arXiv commentAccepted for publication in MNRAS Letters

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Cited by in corpus (13)

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• The Effect of Transient Accretion on the Spin-Up of Millisecond Pulsars
• Impact of the equation-of-state -- gravity degeneracy on constraining the nuclear symmetry energy from astrophysical observables
• Compiled Properties of Nucleonic Matter and Nuclear and Neutron Star Models from Non-Relativistic and Relativistic Interactions
• On the last stable orbit around rapidly rotating neutron stars
• Millisecond radio pulsars with known masses: parameter values and equation of state models
• New quasi-universal relations for static and rapid rotating neutron stars
• Formation of redbacks via accretion induced collapse
• Assessing the complexity of orbital parameters after asymmetric kick in binary pulsars
• Universal behavior of compact star based upon gravitational binding energy
• Investigation of Some Physical Properties of Accretion Induced Collapse in Producing Millisecond Pulsars
• The binding energy produced within the framework of the accretion of millisecond pulsars
• The Role of Strong Gravity and the Nuclear Equation of State on Neutron-Star Common-Envelope Accretion