Equation of state for neutron stars in SU(3) flavor symmetry

Abstract

Using several relativistic mean field models (such as GM1, GM3, NL3, TM1, FSUGold and IU-FSU) as well as the quark-meson coupling model, we calculate the particle fractions, the equation of state, the maximum mass and radius of a neutron star within relativistic Hartree approximation. In determining the couplings of the isoscalar, vector mesons to the octet baryons, we examine the extension of SU(6) spin-flavor symmetry to SU(3) flavor symmetry. Furthermore, we consider the strange (${\sigma }^{\ast }$ and $\varphi$) mesons, and study how they affect the equation of state. We find that the equation of state in SU(3) symmetry can sustain a neutron star with mass of $(1.8\sim 2.1)M_{\odot }$ even if hyperons exist inside the core. In addition, the strange vector ($\varphi$) meson and the variation of baryon structure in matter also play important roles in supporting a massive neutron star.

28 pages, 12 figures, 5 tables

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