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Title: Role of isospin physics in supernova matter and neutron stars

Abstract

We investigate the liquid-gas phase transition of hot protoneutron stars shortly after their birth following supernova explosion and the composition and structure of hyperon-rich (proto)neutron stars within a relativistic mean-field model where the nuclear symmetry energy was constrained from the measured neutron skin thickness of finite nuclei. Light clusters are abundantly formed with increasing temperature well inside the neutrino-sphere for a uniform supernova matter. Liquid-gas phase transition is found to suppress the cluster yield within the coexistence phase as well as decrease considerably the neutron-proton asymmetry over a wide density range. We find symmetry energy has a modest effect on the boundaries and the critical temperature for the liquid-gas phase transition, and the composition depends more sensitively on the number of trapped neutrinos and temperature of the protoneutron star. The influence of hyperons in the dense interior of stars makes the overall equation of state soft. However, neutrino trapping distinctly delays the appearance of hyperons because of an abundance of electrons. We also find that a softer symmetry energy further makes the onset of hyperon less favorable. The resulting structures of the (proto)neutron stars with hyperons and with liquid-gas phase transition are discussed.

Authors:
;  [1]
  1. Department of Nuclear and Atomic Physics, Tata Institute of Fundamental Research, Homi Bhabha Road, Mumbai 400005 (India)
Publication Date:
OSTI Identifier:
21499218
Resource Type:
Journal Article
Journal Name:
Physical Review. C, Nuclear Physics
Additional Journal Information:
Journal Volume: 82; Journal Issue: 5; Other Information: DOI: 10.1103/PhysRevC.82.055802; (c) 2010 The American Physical Society; Journal ID: ISSN 0556-2813
Country of Publication:
United States
Language:
English
Subject:
72 PHYSICS OF ELEMENTARY PARTICLES AND FIELDS; 79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ASYMMETRY; CRITICAL TEMPERATURE; ELECTRONS; EQUATIONS OF STATE; EXPLOSIONS; HYPERONS; ISOSPIN; MEAN-FIELD THEORY; NEUTRINOS; NEUTRON STARS; NEUTRONS; NUCLEI; PHASE TRANSFORMATIONS; PROTONS; RELATIVISTIC RANGE; SUPERNOVAE; SYMMETRY; BARYONS; BINARY STARS; ELEMENTARY PARTICLES; ENERGY RANGE; EQUATIONS; ERUPTIVE VARIABLE STARS; FERMIONS; HADRONS; LEPTONS; MASSLESS PARTICLES; NUCLEONS; PARTICLE PROPERTIES; PHYSICAL PROPERTIES; STARS; STRANGE PARTICLES; THERMODYNAMIC PROPERTIES; TRANSITION TEMPERATURE; VARIABLE STARS

Citation Formats

Sharma, Bharat K, and Pal, Subrata. Role of isospin physics in supernova matter and neutron stars. United States: N. p., 2010. Web. doi:10.1103/PHYSREVC.82.055802.
Sharma, Bharat K, & Pal, Subrata. Role of isospin physics in supernova matter and neutron stars. United States. https://doi.org/10.1103/PHYSREVC.82.055802
Sharma, Bharat K, and Pal, Subrata. 2010. "Role of isospin physics in supernova matter and neutron stars". United States. https://doi.org/10.1103/PHYSREVC.82.055802.
@article{osti_21499218,
title = {Role of isospin physics in supernova matter and neutron stars},
author = {Sharma, Bharat K and Pal, Subrata},
abstractNote = {We investigate the liquid-gas phase transition of hot protoneutron stars shortly after their birth following supernova explosion and the composition and structure of hyperon-rich (proto)neutron stars within a relativistic mean-field model where the nuclear symmetry energy was constrained from the measured neutron skin thickness of finite nuclei. Light clusters are abundantly formed with increasing temperature well inside the neutrino-sphere for a uniform supernova matter. Liquid-gas phase transition is found to suppress the cluster yield within the coexistence phase as well as decrease considerably the neutron-proton asymmetry over a wide density range. We find symmetry energy has a modest effect on the boundaries and the critical temperature for the liquid-gas phase transition, and the composition depends more sensitively on the number of trapped neutrinos and temperature of the protoneutron star. The influence of hyperons in the dense interior of stars makes the overall equation of state soft. However, neutrino trapping distinctly delays the appearance of hyperons because of an abundance of electrons. We also find that a softer symmetry energy further makes the onset of hyperon less favorable. The resulting structures of the (proto)neutron stars with hyperons and with liquid-gas phase transition are discussed.},
doi = {10.1103/PHYSREVC.82.055802},
url = {https://www.osti.gov/biblio/21499218}, journal = {Physical Review. C, Nuclear Physics},
issn = {0556-2813},
number = 5,
volume = 82,
place = {United States},
year = {Mon Nov 15 00:00:00 EST 2010},
month = {Mon Nov 15 00:00:00 EST 2010}
}