Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 481, Issue 3, Pages 2994-3026Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/sty2413
Keywords
dense matter; equation of state; stars: neutron
Categories
Funding
- Natural Sciences and Engineering Research Council (Canada)
- Russian Foundation for Basic Research [16-29-13009-ofi-m]
- Fonds de la Recherche Scientifique (Belgium) [CDR-J.0187.16, CDR-J.0115.18. SG]
- European Cooperation in Science and Technology (COST) Actions [MP1304, CA16214]
- Fonds de la Recherche Scientifique (Belgium)
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The theory of the nuclear energy-density functional is used to provide a unified and thermodynamically consistent treatment of all regions of cold non-accreting neutron stars. In order to assess the impact of our lack of complete knowledge of the density dependence of the symmetry energy on the constitution and the global structure of neutron stars, we employ four different functionals. All of them were precision fitted to essentially all the nuclear mass data with the Hartree-Fock-Bogoliubov method and two different neutron-matter equations of state based on realistic nuclear forces. For each functional, we calculate the composition, the pressure-density relation, and the chemical potentials throughout the star. We show that uncertainties in the symmetry energy can significantly affect the theoretical results for the composition and global structure of neutron stars. To facilitate astrophysical applications, we construct analytic fits to our numerical results.
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