Magnetic, thermal and rotational evolution of isolated neutron stars

TL;DR

This review discusses the magneto-thermal evolution of neutron stars, emphasizing numerical modeling, microphysical properties, and recent advances in 3D simulations to understand their magnetic and thermal history.

Contribution

It provides a comprehensive overview of the theory, numerical techniques, and benchmark tests for modeling neutron star magnetic and thermal evolution, including recent 3D developments.

Findings

Summarizes key results from axisymmetric models.

Highlights recent advances in 3D simulations.

Provides benchmark tests for future code development.

Abstract

The strong magnetic field of neutron stars is intimately coupled to the observed temperature and spectral properties, as well as to the observed timing properties (distribution of spin periods and period derivatives). Thus, a proper theoretical and numerical study of the magnetic field evolution equations, supplemented with detailed calculations of microphysical properties (heat and electrical conductivity, neutrino emission rates) is crucial to understand how the strength and topology of the magnetic field vary as a function of age, which in turn is the key to decipher the physical processes behind the varied neutron star phenomenology. In this review, we go through the basic theory describing the magneto-thermal evolution models of neutron stars, focusing on numerical techniques, and providing a battery of benchmark tests to be used as a reference for present and future code developments. We summarize well-known results from axisymmetric cases, give a new look at the latest 3D advances, and present an overview of the expectations for the field in the coming years.