Evolution of the Magnetic Field in Accreting Neutron Stars

TL;DR

This paper investigates how accretion in binary systems affects the magnetic field evolution of neutron stars, aiming to explain the formation of millisecond pulsars through various magnetic flux evolution models and observational comparisons.

Contribution

It explores multiple models of magnetic flux evolution in accreting neutron stars, including crustal and core flux, and compares these models with observational data to understand millisecond pulsar formation.

Findings

Diamagnetic screening influences the neutron star's magnetic field during accretion.

Crustal magnetic flux evolution models align with observed magnetic field decay.

Initial core flux location has significant observational implications.

Abstract

There has been sufficient observational indication suggesting a causal connection between the binary history of neutron stars and the evolution of their magnetic field. In particular, it is believed that the generation of the low-field millisecond pulsars is a consequence of the processing of normal high-field neutron stars in binary systems. We try to understand the mechanism of field evolution in neutron stars that are members of binary systems with an aim to understand the problem of millisecond pulsar generation. To this end we have looked at four related problems : i. the effect of diamagnetic screening on the final field of a neutron star accreting material from its binary companion; ii. evolution of magnetic flux located in the crust of an accreting neutron star; iii. application of the above-mentioned model to real systems and a comparison with observations; iv. an investigation into the consequences of magnetic flux being initially located in the core of the star and its observational implications.