The role of mass, equation of state and superfluid reservoir in large pulsar glitches

TL;DR

This study investigates how pulsar glitch observations can constrain neutron star masses, emphasizing the importance of superfluid regions and the equation of state in modeling neutron star internal dynamics.

Contribution

It provides an analysis of mass constraints based on pulsar glitches, highlighting the sensitivity to superfluid extent and internal structure assumptions.

Findings

Mass constraints depend on the superfluid region extending inside the outer core.

Stable mass estimates are achieved when the superfluid extends to densities above nuclear saturation.

Mass estimates are consistent with observed neutron star masses within certain superfluid configurations.

Abstract

Observations of pulsar glitches may provide insights on the internal physics of neutron stars and recent studies show how it is in principle possible to constrain pulsar masses with timing observations. The reliability of these estimates depend on the current uncertainties about the structure of neutron stars and on our ability to model the dynamics of the superfluid neutrons in the internal layers. We assume a simplified model for the rotational dynamics of a neutron star and estimate an upper bound to the mass of 25 pulsars from their largest glitch and average activity: the aim is to understand to which extent the mass constraints are sensitive to the choice of the unknown structural properties of neutron stars, like the extension of the superfluid region and the equation of state. Reasonable values, within the range measured for neutron star masses, are obtained only if the superfluid domain extends for at least a small region inside the outer core, which is compatible with calculations of the neutron S-wave pairing gap. Moreover, the mass constraints stabilise when the superfluid domain extends to densities over nuclear saturation, irrespective of the equation of state tested.