Equation of state of the neutron star matter, and the nuclear symmetry energy

Abstract

The nuclear mean-field potentials obtained in the Hartree-Fock method with different choices of the in-medium nucleon-nucleon (NN) interaction have been used to study the equation of state (EOS) of the neutron star (NS) matter. The EOS of the uniform NS core has been calculated for the np$e\mu$ composition in the $\beta$-equilibrium at zero temperature, using version Sly4 of the Skyrme interaction as well as two density-dependent versions of the finite-range M3Y interaction (CDM3Y$n$ and M3Y-P$n$), and versions D1S and D1N of the Gogny interaction. Although the considered effective NN interactions were proven to be quite realistic in numerous nuclear structure and/or reaction studies, they give quite different behaviors of the symmetry energy of nuclear matter at supranuclear densities that lead to the \emph{soft} and \emph{stiff} scenarios discussed recently in the literature. Different EOS's of the NS core and the EOS of the NS crust given by the compressible liquid drop model have been used as input of the Tolman-Oppenheimer-Volkov equations to study how the nuclear symmetry energy affects the model prediction of different NS properties, like the cooling process as well as the gravitational mass, radius, and moment of inertia.

arXiv commentTo be published in Physical Review C

References in corpus (45)

• The equation of state for nucleon matter and neutron star structure
• Determination of the Equation of State of Dense Matter
• The Physics of Neutron Stars
• Neutron Star Observations: Prognosis for Equation of State Constraints
• Recent Progress and New Challenges in Isospin Physics with Heavy-Ion Reactions
• A unified equation of state of dense matter and neutron star structure
• The Equation of State from Observed Masses and Radii of Neutron Stars
• Reaction Dynamics with Exotic Beams
• Neutron-Rich Nuclei in Heaven and Earth
• Constraints on the density dependence of the symmetry energy
• Minimal Cooling of Neutron Stars: A New Paradigm
• Nuclear symmetry energy probed by neutron skin thickness of nuclei
• Isospin Physics in Heavy-Ion Collisions at Intermediate Energies
• Determination of the stiffness of the nuclear symmetry energy from isospin diffusion
• Neutron Radii in Mean-Field Models
• Astrophysical Measurement of the Equation of State of Neutron Star Matter
• Gravitationally redshifted absorption lines in the X-ray burst spectra of a neutron star
• Constraints on the high-density nuclear equation of state from the phenomenology of compact stars and heavy-ion collisions
• Constraining the Equation of State with Moment of Inertia Measurements
• Circumstantial evidence for a soft nuclear symmetry energy at supra-saturation densities
• Asymmetric Nuclear Matter from Extended Brueckner-Hartree-Fock Approach
• Surface Symmetry Energy
• The Giant Dipole Resonance as a quantitative constraint on the symmetry energy
• Density dependence of the symmetry energy and the nuclear equation of state: A Dynamical and Statistical model perspective
• Isospin fractionation and isoscaling in dynamical nuclear collisions
• Nuclear rainbow scattering and nucleus-nucleus potential
• A New Equation of State for Astrophysical Simulations
• Incompressibility of neutron-rich matter
• The Double Pulsar J0737--3039: Testing the Neutron Star Equation of State
• Hartree-Fock approach to nuclear matter and finite nuclei with M3Y-type nucleon-nucleon interactions
• Dirac-Brueckner-Hartree-Fock calculations for isospin asymmetric nuclear matter based on improved approximation schemes
• Microscopic calculation of the equation of state of nuclear matter and neutron star structure
• Equation of State of Nuclear Matter at high baryon density
• Mean-field approach to nuclear structure with semi-realistic nucleon-nucleon interactions
• Constraints on the density dependence of the symmetry energy from heavy ion collisions
• Validating relativistic models of nuclear structure against theoretical, experimental, and observational constraints
• Folding model study of the isobaric analog excitation: isovector density dependence, Lane potential and nuclear symmetry energy
• Versatility of field theory motivated nuclear effective Lagrangian approach
• Isospin dependence of 6He+p optical potential and the symmetry energy
• A method of implementing Hartree-Fock calculations with zero- and finite-range interactions
• Nuclear equation of state at high baryonic density and compact star constraints
• Isospin dependent properties of asymmetric nuclear matter
• Neutron star cooling - a challenge to the nuclear mean field
• Neutron transition strengths of $2_1^{+}$ states in the neutron rich Oxygen isotopes determined from inelastic proton scattering
• Constraining the density dependence of the symmetry energy in the nuclear equation of state using heavy ion beams

Cited by in corpus (25)

• Density dependence of the symmetry energy from neutron skin thickness in finite nuclei
• On the Induced Gravitational Collapse of a Neutron Star to a Black Hole by a Type Ib/c Supernova
• Neutron star equilibrium configurations within a fully relativistic theory with strong, weak, electromagnetic, and gravitational interactions
• Deformation of Ne isotopes in the island-of-inversion region
• Higher-order symmetry energy and neutron star core-crust transition with Gogny forces
• New Gogny interaction suitable for astrophysical applications
• Semi-realistic nucleon-nucleon interactions with improved neutron-matter properties
• Microscopic description of fission in superheavy nuclei with the parametrization D1M${}^{\ast }$ of the Gogny energy density functional
• Thermodynamic properties and shear viscosity over entropy density ratio of nuclear fireball in a quantum-molecular dynamics model
• Sensitivity of neutron to proton ratio toward the high density behavior of symmetry energy in heavy-ion collisions
• Folding model study of the charge-exchange scattering to the isobaric analog state and implication for the nuclear symmetry energy
• Mean-field study of hot beta-stable protoneutron star matter: Impact of the symmetry energy and nucleon effective mass
• Properties of exotic nuclei and their linkage to the nucleonic interaction
• Influence of the single-particle structure on the nuclear surface and the neutron skin
• Understanding the symmetry energy using data from the ALADIN-2000 Collaboration taken at the GSI Large Neutron Detector
• Indirect methods in nuclear astrophysics with relativistic radioactive beams
• Impacts of symmetry energy slope on the oscillation frequencies of neutron stars with short-range correlation and admixed dark matter
• Rearrangement term in the nonlocal folding model of the nucleon optical potential
• Linear Response Theory with finite-range interactions
• Core-crust transition and crustal fraction of moment of inertia in neutron stars
• Nuclear Symmetry Energy and Neutron Skin Thickness of ${}^{208}Pb$ using a finite range effective interaction
• Lee-Yang-inspired energy-density functional including contributions from $p$-wave scattering
• Equation of state of asymmetric nuclear matter and the tidal deformability of neutron star
• Spin-polarized $\beta$-stable neutron star matter: the nuclear symmetry energy and GW170817 constraint
• Folding model approach to the elastic $p{+}^{12,13}$C scattering at low energies and radiative capture ${}^{12,13}$C$(p,\gamma )$ reactions