Precession and glitches in the framework of three-component model of neutron star

TL;DR

This paper models neutron star rotation with a three-component system, explaining observed glitches and long-period precession through interactions between the crust and core components, including pinned superfluid dynamics.

Contribution

It introduces a three-component neutron star model that accounts for both glitches and long-period precession, highlighting the role of pinned superfluid in the core.

Findings

The model explains glitch-like events and precession periods from years to thousands of years.

Pinned superfluid can inject angular momentum suddenly, causing observable glitches.

Long-period precession can coexist with glitch phenomena in the proposed framework.

Abstract

We consider the pulsar rotation assuming that the neutron star consists of crust component (which rotation is observed) and two core components. One of the core components contains pinned superfluid which can, for some reasons, suddenly inject small fraction of stored angular momentum in it. In the framework of this simple model the star can demonstrate glitch-like events together with long period precession (with period $1-10^{4}$ years).