Equation of state for neutron stars: Hyperon mixing in SU(3) flavor symmetry
classification
⚛️ nucl-th
astro-ph.HE
keywords
neutronequationflavorstarstarsstatesymmetrycore
read the original abstract
Using various kinds of relativistic mean-field models as well as the quark-meson coupling model, we study in detail the properties of neutron stars. We find that the equation of state in SU(3) flavor symmetry can support a neutron star with mass of $(1.8 \sim 2.1) M_{\odot}$ even if hyperons exist inside the core of a neutron star.
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