Internal composition of proto-neutron stars under strong magnetic fields

B. Franzon, V. Dexheimer, and S. Schramm
Phys. Rev. D 94, 044018 – Published 10 August 2016

Abstract

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.

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  • Received 13 June 2016

DOI:https://doi.org/10.1103/PhysRevD.94.044018

© 2016 American Physical Society

Physics Subject Headings (PhySH)

  1. Research Areas
  1. Physical Systems
Gravitation, Cosmology & Astrophysics

Authors & Affiliations

B. Franzon*

  • Frankfurt Institute for Advanced Studies, Ruth-Moufang—1 60438 Frankfurt am Main, Germany

V. Dexheimer

  • Department of Physics, Kent State University, Kent, Ohio 44242 USA

S. Schramm

  • Frankfurt Institute for Advanced Studies, Ruth-Moufang—1 60438 Frankfurt am Main, Germany

  • *franzon@fias.uni-frankfurt.de
  • vdexheim@kent.edu
  • schramm@fias.uni-frankfurt.de

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Issue

Vol. 94, Iss. 4 — 15 August 2016

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