Neutron Stars with Hyperons subject to Strong Magnetic Field

TL;DR

This paper investigates how strong magnetic fields and hyperons influence the equation of state, structure, and cooling processes of neutron stars, revealing significant effects on their mass and composition.

Contribution

It provides a detailed analysis of the impact of magnetic fields and hyperons on neutron star properties using a relativistic model, highlighting their importance in magnetar physics.

Findings

Strong magnetic fields can increase neutron star mass by over 10%.

Hyperons and magnetic fields significantly affect the star's chemical composition and cooling processes.

Magnetars can reach masses up to 2.48 solar masses, explaining the observed mass distribution.

Abstract

Neutron stars are one of the most exotic objects in the universe and a unique laboratory to study the nuclear matter above the nuclear saturation density. In this work, we study the equation of state of the nuclear matter within a relativistic model subjected to a strong magnetic field. We then apply this EoS to study and describe some of the physical characteristics of neutron star, especially the mass-radius relation and chemical compositions. To study the influence of a the magnetic field and the hyperons in the stellar interior, we consider altogether four solutions: two different values of magnetic field to obtain a weak and a strong influence, and two configurations: a family of neutron stars formed only by protons, electrons and neutrons and a family formed by protons, electrons, neutrons, muons and hyperons. The limit and the validity of the results found are discussed with some care. In all cases the particles that constitute the neutron star are in $\beta$ equilibrium and zero total net charge. Our work indicates that the effect of a strong magnetic field has to be taken into account in the description of magnetars, mainly if we believe that there are hyperons in their interior, in which case, the influence of the magnetic field can increase the mass by more than 10%. We have also seen that although a magnetar can reach 2.48$M_{\odot}$, a natural explanation of why we do not know pulsars with masses above 2.0$M_{\odot}$ arises. We also discuss how the magnetic field affects the strangeness fraction in some standard neutron star masses and, to conclude our paper, we revisit the direct URCA process related to the cooling of the neutron stars and show how it is affected by the hyperons and the magnetic field.