The role of equation of state on the spin-up of millisecond pulsars

TL;DR

This paper explores how the equation of state influences the spin-up process of millisecond pulsars, comparing neutron star and strangeon star models, and highlights the impact of magnetic fields and accreted mass on their spin evolution.

Contribution

It introduces a combined approach using spin-up conditions, angular momentum transfer, and magnetic field evolution to constrain MSP properties in different star models.

Findings

Magnetic fields more significantly impede MSP spin-up in neutron stars than in strangeon stars.

Low-mass strangeon stars can spin faster than neutron stars of the same mass with equal accreted mass.

Accurate measurements of low-mass MSPs can better constrain the equation of state of pulsars.

Abstract

Millisecond pulsars (MSPs) are recycled pulsars which have been spun-up due to mass accretion during the phase of mass exchange in binaries. Although the interactions with companion stars play important roles on the spin-up process, the global properties of pulsars determined by the equation of state (EoS), such as mass, radius and the moment of inertia, should also play a role. We investigate the spin-up of MSPs in neutron star (NS) and strangeon star (SS) models, both of which have passed the tests by the existence of high-mass pulsars and the tidal deformability of GW~170817. Combining the spin-up condition and the transferred angular momentum, and taking into account the evolution of magnetic field strength during accretion, we can constrain the spin-period and mass of an MSP. Our results show that the impeding effect of magnetic field on the spin-up of MSPs would be more significant for NSs than for SSs, especially for the ones with low masses. In the low-mass ($M$ below or around about $1.2 M_\odot$) case, an SS can spin faster than an NS of the same mass by accreting the same amount of mass. Finding more low-mass and fully recycled MSPs, with accurate mass-measurement and better constraints on the amount of accreted mass, could help to put more strict constraints on the EoS of pulsars.