Rotational evolution of deformed magnetized neutron stars: implications for obliquity distribution and braking indices statistics

TL;DR

This paper models the rotational evolution of deformed, magnetized neutron stars considering magnetic field decay and free precession, revealing effects on obliquity distribution and pulsar braking indices.

Contribution

It introduces a comprehensive model of neutron star evolution that includes crust deformations, magnetic field decay, and free precession, explaining observed pulsar properties.

Findings

Broadening of magnetic obliquity angle distribution.

Formation of a limit-cycle regime in rotational axis behavior.

Periodic oscillations in pulsar braking indices.

Abstract

The rotational evolution of a strongly magnetized neutron star (NS), accreting or isolated, is driven by external torques of different nature. In addition to the torques, even the tiniest deformations of the NS crust can affect its rotation through asymmetries in its inertia tensor. Several factors may be responsible for the deformations, including strong magnetic fields, internal stresses, or local heating. The main effect produced by the deformations is the so-called free precession: the motion of the rotational axis with respect to the crust. We consider the evolution of a triaxially deformed isolated NS with a strong dipolar magnetic field for a broad range of parameters, taking into account the magnetic field decay. We show that the combination of pulsar torques and free precession results in a considerable broadening of the distribution of magnetic obliquity angles (the angle between the magnetic and rotational axes) and creates a population of objects where the rotational axis does not align with the magnetic axis at all but enters a limit-cycle regime. The combination of free precession and magnetic torques can also explain the observed distribution in pulsar braking indices by creating a periodic oscillation in the magnetic obliquity.