Evolutions of Neutron Stars and their Magnetic Fields

TL;DR

This paper reviews the magnetic field estimations of neutron stars, compares theoretical and observational data, discusses magnetic field screening models, and analyzes the nature of soft gamma repeaters and magnetars.

Contribution

It provides a comprehensive comparison of magnetic field estimates from various observational methods and discusses models explaining magnetic field screening in neutron stars.

Findings

Magnetic fields of recycled pulsars are 2-4 orders of magnitude smaller than single pulsars.

Discrepancies exist between cyclotron line estimates and observational data for some X-ray pulsars.

Relativistic dipole radiation may explain certain cyclotron feature anomalies.

Abstract

Estimations of magnetic fields of neutron stars, observed as radio and X-ray pulsars, are discussed. It is shown, that theoretical and observational values for different types of radiopulsars are in good correspondence. Radiopulsars in close binaries and millisecond pulsars, which have passed the stage of disk accretion (recycled radiopulsars), have magnetic fields 2-4 orders of magnitude smaller than ordinary single pulsars. Most probably, the magnetic field of the neutron star was screened by the infalling material. Several screening models are considered. Formation of single recycled pulsars loosing its companion is discussed. Magnetic fields of some X-ray pulsars are estimated from the cyclotron line energy. In the case of Her X-1 this estimation exceeds considerably the value of its magnetic field obtained from long term observational data related to the beam structure evolution. Another interpretation of the cyclotron feature, based on the relativistic dipole radiation mechanism, could remove this discrepancy. Observational data about soft gamma repeaters and their interpretation as magnetars are critically analyzed.