Neutron star properties: Constraining the nuclear matter EoS
arXiv:1904.04386 · doi:10.1063/1.5117812
Abstract
We examine the influence of the density dependence of the symmetry energy on several properties of neutron stars. In particular, we study the constraints set on the nuclear matter equation of state by the values of the tidal deformability and neutron star radius, using a diverse set of relativistic and non-relativistic mean field models consistent with bulk properties of finite nuclei and the observed lower bound on the maximum mass of neutron star. The tidal deformability and radius show a strong correlation with specific linear combinations of the isoscalar and isovector nuclear matter parameters associated with the EoS. Such correlations suggest that a precise value of the radius or the tidal deformability can put tight bounds on several EoS parameters, in particular, on the slope of the incompressibility and the curvature of the symmetry energy. We show that the density dependence of the symmetry energy has a direct influence on the amount of strangeness inside cold dense matter and, consequently, on the direct Urca process and cooling of neutron stars. We explain the low luminosity of SAX 1808.4-3658 as a result of hyperonic direct Urca processes. Finally, we discuss the strong influence of the density dependence of the symmetry energy on the extension of the crust-core transition region of a magnetized neutron star. The increase of the crust and its of complexity, due to the magnetic field effect, may have a role on the glitch mechanism or on the magnetic field decay.
10 pages, 6 figures, to appear in the AIP Conference Proceedings of the Xiamen-CUSTIPEN Workshop on the EOS of Dense Neutron-Rich Matter in the Era of Gravitational Wave Astronomy (January 3 - 7, 2019, Xiamen, China)
References in corpus (29)
- 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
- GW170817: Measurements of Neutron Star Radii and Equation of State
- Tidal Love numbers of neutron stars
- Tidal Deformabilities and Radii of Neutron Stars from the Observation of GW170817
- The NANOGrav 11-year Data Set: High-precision timing of 45 Millisecond Pulsars
- GW170817: Joint Constraint on the Neutron Star Equation of State from Multimessenger Observations
- Neutron skins and neutron stars in the multi-messenger era
- A critical examination of constraints on the equation of state of dense matter obtained from GW170817
- Building relativistic mean field models for finite nuclei and neutron stars
- GW170817: constraining the nuclear matter equation of state from the neutron star tidal deformability
- Core-crust transition in neutron stars: predictivity of density developments
- Crustal Entrainment and Pulsar Glitches
- Density dependence of the nuclear symmetry energy: a microscopic perspective
- Neutron star tidal deformabilities constrained by nuclear theory and experiment
- Estimation of the effect of hyperonic three-body forces on the maximum mass of neutron stars
- Equation of state and thickness of the inner crust of neutron stars
- Extracting Nuclear Symmetry Energies at High Densities from Observations of Neutron Stars and Gravitational Waves
- Neutron star equation of state from the quark level in the light of GW170817
- The Equation of State for the Nucleonic and Hyperonic Core of Neutron Stars
- Strong correlations of neutron star radii with the slopes of nuclear matter incompressibility and symmetry energy at saturation
- Nuclear symmetry energy and core-crust transition in neutron stars: a critical study
- Statistical theory of thermal evolution of neutron stars
- Hyperonic stars and the symmetry energy
- Cooling of Small and Massive Hyperonic Stars
- Influence of the symmetry energy on nuclear pasta in neutron star crusts
- Crust-core transition of a neutron star: effects of the symmetry energy and temperature under strong magnetic fields
- Quantum Key Distribution With several intercept-resend attacks Via A Depolarizing Channel