Equation of state for neutron stars: Hyperon mixing in SU(3) flavor   symmetry
  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. 
Tsuyoshi Miyatsu, Myung-Ki Cheoun and Koichi Saito
nucl-th astro-ph.HE