2016/06/30 by B. Franzon, V. Dexheimer, Verônica Dexheimer +1 · 1 citation
Earth and Planetary Sciences · Physics and Astronomy · #Astrophysics #Baryon #Hadron #High-pressure geophysics and materials #Magnetic field #Neutrino #Neutron #Neutron star #Nuclear physics #Physics #Population #Pulsars and Gravitational Waves Research #Quantum mechanics #Quantum, superfluid, helium dynamics #Stars #Strangeness #astro-ph.HE #nucl-th
paper · pdf · doi:10.1103/physrevd.94.044018
published as Phys. Rev. D 94, 044018 (2016) · Accepted for publication in PRD
arxiv created 2016/07/27 · openalex publication_date 2016/08/10 · arxiv updated 2016/08/17 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
In this work, we study the effects of magnetic fields and rotation on the structure and composition of proto-neutron stars. A hadronic chiral SU(3) model is applied to cold neutron stars 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.