The influence of small-scale magnetic field on the evolution of inclination angle and precession damping in the framework of 3-component model of neutron star

TL;DR

This paper models neutron star evolution considering a three-component system with small-scale magnetic fields, revealing that few pinned superfluid vortices align better with observed pulsar behaviors like glitches and precession.

Contribution

It introduces a 3-component neutron star model incorporating small-scale magnetic fields and analyzes their effects on inclination angle evolution and precession damping.

Findings

Small-scale magnetic fields influence star braking.

Few pinned superfluid vortices match observational data.

Star can exhibit glitch-like events with long precession periods.

Abstract

The evolution of inclination angle and precession damping of radio pulsars is considered. It is assumed that the neutron star consists of 3 "freely" rotating components: the crust and two core components, one of which contains pinned superfluid vortices. We suppose that each component rotates as a rigid body. Also the influence of the small-scale magnetic field on the star's braking process is examined. Within the framework of this model the star simultaneously can have glitch-like events combined with long-period precession (with periods $10-10^{4}$ years). It is shown that the case of the small quantity of pinned superfluid vortices seems to be more consistent with observations.