The internal composition of proto-neutron stars under strong magnetic fields

Abstract

In this work, we study the effects of magnetic fields and rotation on the structure and composition of proto-neutron stars (PNS's). A hadronic chiral SU(3) model is applied to cold neutron stars (NS) and proto-neutron stars with trapped neutrinos and at fixed entropy per baryon. We obtain general relativistic solutions for neutron and proto-neutron stars endowed with a poloidal magnetic field by solving Einstein-Maxwell field equations in a self-consistent way. As the neutrino chemical potential decreases in value over time, this alters the chemical equilibrium and the composition inside the star, leading to a change in the structure and in the particle population of these objects. We find that the magnetic field deforms the star and significantly alters the number of trapped neutrinos in the stellar interior, together with strangeness content and temperature in each evolution stage.

Accepted for publication in PRD

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Cited by in corpus (11)

• General relativistic models for rotating magnetized neutron stars in conformally flat spacetime
• Many-body forces in magnetic neutron stars
• Limiting magnetic field for minimal deformation of a magnetised neutron star
• Effects of Magnetic Fields in Hot White Dwarfs
• Quasi-universality of the magnetic deformation of neutron stars in general relativity and beyond
• AR Scorpii and possible gravitational wave radiation from pulsar white dwarfs
• Axisymmetric equilibrium models for magnetised neutron stars in Scalar-Tensor Theories
• The property difference between the neutron star PSR J0348+0432 and its proto neutron star
• Hyperons and $\Delta$'s in rotating protoneutron stars: Global properties
• Methods for relativistic self-gravitating fluids: From binary neutron stars to black hole-disks and magnetized rotating neutron stars
• Rotating neutron stars with chaotic magnetic fields in general relativity and Rastall gravity