Pulsar glitch and nuclear EoS: Applicability of superfluid model

Abstract

In this contribution, we have made use of the contemporary equation of states (EOSs) for the complete neutron star structure, and confronted them with one particular glitch constrain for the crustal moment of inertia (MOI). We find that with these EOSs, the radii of three millisecond pulsars selected by NICER: PSR J0437-4715, PSR J1614-2230, PSR J0751+1807, are all around 12.5 km. Also, a star with $M\lesssim 1.55M_{\odot }$ would fulfill the MOI calculation for glitch constrain with the latest neutron superfluidity density, and the glitch crisis might not be present.

proceeding prepared for IAU Symposium 337: 50 Years of Pulsars, Jodrell Bank Observatory, United Kingdom, 4-8 September 2017; In press

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Cited by in corpus (1)

• Unified neutron star EOSs and neutron star structures in RMF models