Exploring universal characteristics of neutron star matter with relativistic \textit{ab initio} equations of state

Abstract

Starting from the relativistic realistic nucleon-nucleon ($NN$) interactions, a newly developed relativistic \textit{ab initio} method, i.e., the relativistic Brueckner-Hartree-Fock (RBHF) theory in the full Dirac space is employed to study the neutron star properties. First, the one-to-one correspondence relation for gravitational redshift and mass is established and used to infer the mass of isolated neutron stars combining the gravitational redshift measurements. Next, the ratio of the moment of inertia $I$ to $M{R}^2$ as a function of the compactness $M/R$ is obtained, which is consistent with the universal relations in the literature. The moment of inertia for $1.338M_{\odot }$ pulsar PSR J0737-3039A $I_{1.338M_{\odot }}$ is predicted to be 1.356$\times 10^{45}$, 1.381$\times 10^{45}$, and $1.407\times 10^{45}\mathrm{g}\mathrm{c}{\mathrm{m}}^2$ by the RBHF theory in the full Dirac space with $NN$ interactions Bonn A, B, and C, respectively. Finally, the quadrupole moment of neutron star is calculated under the slow-rotation and small-tidal-deformation approximation. The equation of states constructed by the RBHF theory in the full Dirac space, together with those by the projection method and momentum-independence approximation, conform to universal $I$-Love-$Q$ relations as well. By combing the tidal deformability from GW170817 and the universal relations from relativistic \textit{ab initio} methods, the moment of inertia of neutron star with 1.4 solar mass is also deduced as $I_{1.4M_{\odot }}=1.22_{-0.25}^{+0.40}\times 10^{45}\mathrm{g}\mathrm{c}{\mathrm{m}}^2$.

arXiv comment21 pages, 5 figures

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• Speed of sound bounds and first-order phase transitions in compact stars
• Microscopic optical potential from the relativistic Brueckner-Hartree-Fock theory: Proton-nucleus scattering
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• Effect of symmetry energy on properties of rapidly rotating neutron stars and universal relations
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• Equation-of-State Independent Relations in Rapidly Rotating Hybrid Stars
• Toward a Unified Understanding of the Dense Matter Equation of State