Properties of neutron star described by a relativistic $abinitio$ model

Abstract

Properties of neutron star are investigated by an available relativistic $abinitio$ method, i.e., the relativistic Brueckner-Hartree-Fock (RBHF) model, with the latest high-precision relativistic charge-dependent potentials, pvCD-Bonn A, B, C. The neutron star matter is solved within the beta equilibrium and charge neutrality conditions in the framework of RBHF model. Comparing to the conventional treatment, where the chemical potential of lepton was approximately represented by the symmetry energy of nuclear matter, the equation of state (EOS) of neutron star matter in the present self-consistent calculation with pvCD-Bonn B has striking difference above the baryon number density $n_b=0.55$ fm${}^{-3}$. However, these differences influence the global properties of neutron star only about $1\%\sim 2\%$. Then, three two-body potentials pvCD-Bonn A, B, C, with different tensor components, are systematically applied in RBHF model to calculate the properties of neutron star. It is found that the maximum masses of neutron star are around $2.21\sim 2.30M_{\odot }$ and the corresponding radii are $R=11.18\sim 11.72$ km. The radii of $1.4M_{\odot }$ neutron star are predicated as $R_{1.4}=12.34\sim 12.91$ km and their dimensionless tidal deformabilities are ${\Lambda }_{1.4}=485\sim 626$. Furthermore, the direct URCA process in neutron star cooling will happen from $n_b=0.414\sim 0.530$ fm${}^{-3}$ with the proton fractions, $Y_p=0.136\sim 0.138$. All of the results obtained from RBHF model only with two-body pvCD-Bonn potentials completely satisfy various constraints from recent astronomical observations of massive neutron stars, gravitational wave detection (GW 170817), and mass-radius simultaneous measurement (NICER).

arXiv comment15 pages, 11 figures, 2 tables, accepted by Astrophys. J

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Cited by in corpus (6)

• Neutron star tidal deformability and equation of state constraints
• The possibility of the secondary object in GW190814 as a neutron star
• Nuclear matter in relativistic Brueckner-Hartree-Fock theory with Bonn potential in the full Dirac space
• Nuclear Matter and Neutron Stars from Relativistic Brueckner-Hartree-Fock Theory
• Nonparametric model for the equations of state of neutron star from deep neural network
• Hadron-quark phase transition in neutron star by combining the relativistic Brueckner-Hartree-Fock theory and Dyson-Schwinger equation approach