The Magnetic Field Distribution in Strongly Magnetized Neutron Stars

TL;DR

This paper refines the understanding of magnetic field profiles in strongly magnetized neutron stars, showing quadratic growth with baryon chemical potential and complex behavior with density, using self-consistent models across various matter compositions.

Contribution

It provides a more accurate modeling of magnetic field distribution in neutron stars by incorporating realistic matter models and solving Einstein-Maxwell equations self-consistently.

Findings

Magnetic fields increase quadratically with baryon chemical potential.

Magnetic field growth with baryon density is complex and model-dependent.

Self-consistent solutions reveal nuanced magnetic field profiles.

Abstract

In this work, we expand on a previously reported realistic calculation of the magnetic field profile for the equation of state inside strongly magnetized neutron stars. In addition to showing that magnetic fields increase quadratically with increasing baryon chemical potential of magnetized matter (instead of exponentially, as previously assumed), we show here that the magnetic field increase with baryon number density is more complex and harder to model. We do so by the analysis of several different realistic models for the microscopic description of matter in the star (including hadronic, hybrid and quark models) combined with general relativistic solutions by solving Einstein-Maxwell's field equations in a self-consistent way for stars endowed with a poloidal magnetic field.