Effects of nuclear symmetry energy and equation of state on neutron star properties

Abstract

We study the effects of nuclear symmetry energy on the mass-radius relation and tidal deformability of neutron stars, considering the self-consistency of the equation of state (EOS). We first construct a set of unified EOSs based on relativistic mean-field models with different density dependence of the symmetry energy. For the description of pasta phases appearing in the inner crust of neutron stars, we perform a self-consistent Thomas-Fermi calculation using the same nuclear interaction as that for the uniform matter in the core. To examine possible effects from the self-consistency of the EOS on neutron-star properties, we separately investigate the impacts of crust and core segments. By matching the same core EOS to different crust EOSs, it is found that neutron-star radii are significantly affected by the crust segment. On the other hand, the neutron-star radii are also strongly dependent on the core EOS. However, the correlation between the radius and the symmetry energy slope of the core EOS is opposite to that of the crust EOS. It is likely that the nuclear model with a small slope parameter is favored by recent astrophysical observations.

13 pages, 12 figures

References in corpus (14)

• GW170817: Observation of Gravitational Waves from a Binary Neutron Star Inspiral
• Shapiro delay measurement of a two solar mass neutron star
• A Massive Pulsar in a Compact Relativistic Binary
• Tidal Love numbers of neutron stars
• Relativistic Continuum Hartree Bogoliubov Theory for Ground State Properties of Exotic Nuclei
• GW170817: Joint Constraint on the Neutron Star Equation of State from Multimessenger Observations
• Relativistic effective interaction for nuclei, giant resonances, and neutron stars
• Constraints on the Symmetry Energy Using the Mass-Radius Relation of Neutron Stars
• The symmetry energy at subnuclear densities and nuclei in neutron star crusts
• Nuclear symmetry energy and core-crust transition in neutron stars: a critical study
• Symmetry Energy III: Isovector Skins
• Effects of the symmetry energy on properties of neutron star crusts near the neutron drip density
• Influence of the symmetry energy on nuclear pasta in neutron star crusts
• Phase transitions in Core-Collapse Supernova Matter at sub-saturation densities

Cited by in corpus (5)

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• Influence of the nuclear symmetry energy slope on observables of compact stars with $\Delta$-admixed hypernuclear matter
• Nuclear pasta in hot and dense matter and its influence on the equation of state for astrophysical simulations
• Neutron star deformability with hyperonization in density-dependent relativistic mean-field models