Formation of millisecond pulsars - NS initial mass and EOS constraints

TL;DR

This paper investigates the formation and mass evolution of millisecond pulsars, using observational data, magnetic field interactions, and relativistic models to constrain neutron star equations of state and initial masses.

Contribution

It introduces a comprehensive model combining magnetic field dynamics, accretion processes, and relativistic stellar configurations to better understand pulsar mass formation.

Findings

Reconstructed pre-accretion masses of pulsars considering magnetic and relativistic effects.

Identified the influence of the equation of state on neutron star mass evolution.

Provided constraints on neutron star initial masses based on observational data.

Abstract

Recent measurement of a high millisecond pulsar mass (PSR J1614-2230, 1.97+-0.04 Msun) compared with the low mass of PSR J0751+1807 (1.26+-0.14 Msun) indicates a large span of masses of recycled pulsars and suggests a broad range of neutron stars masses at birth. We aim at reconstructing the pre-accretion masses for these pulsars while taking into account interaction of the magnetic field with a thin accretion disk, magnetic field decay and relativistic 2D solutions for stellar configurations for a set of equations of state. We briefly discuss the evolutionary scenarios leading to the formation of these neutron stars and study the influence of the equation of state.