Insights into the physics of neutron star interiors from pulsar glitches

TL;DR

This paper explores how pulsar glitches reveal the superfluid interior physics of neutron stars, highlighting recent advances and how observations inform our understanding of their internal dynamics.

Contribution

It provides a pedagogical derivation of the formal framework used in glitch studies and discusses recent progress in probing neutron star interiors through observations.

Findings

Superfluid phases influence neutron star dynamics.

Quantum vortices play a key role in glitch mechanisms.

Observations can indirectly probe neutron star interior physics.

Abstract

The presence of superfluid phases in the interior of a neutron star affects its dynamics, as neutrons can flow relative to the non-superfluid (normal) components of the star with little or no viscosity. A probe of superfluidity comes from pulsar glitches, sudden jumps in the observed rotational period of radio pulsars. Most models of glitches build on the idea that a superfluid component of the star is decoupled from the spin-down of the normal component, and its sudden recoupling leads to a glitch. This transition in the strength of the hydrodynamic coupling is explained in terms of quantum vortices (long-lived vortices that are naturally present in the neutron superfluid at the microscopic scale). After introducing some basic ideas, we derive (as a pedagogical exercise) the formal scheme shared by many glitch studies. Then, we apply these notions to present some recent advances and discuss how observations can help us to indirectly probe the internal physics of neutron stars.