Erratum: Hyperons and massive neutron stars: Vector repulsion and SU(3) symmetry [Phys. Rev. C 85, 065802 (2012)]

Figure 2

EoS for different $g_8/g_1$ ratios $z$ within a nonlinear $\sigma \text{−}\omega$ model with an additional $\varphi$ meson and the full baryon octet for the GM1 parameter set. The EoS get stiffer with decreasing $z$.

Figure 3

Mass-radius relations for the EoS displayed in Fig. 2. The maximum mass is obtained for the case $z=0$ where all baryons couple to the vector mesons with equal strengths.

Figure 4

Maximum masses as functions of the $g_8/g_1$ ratio $z$ for the NL3 and GM1 parameter sets. For each parametrization the case of pure nucleonic matter is also displayed.

Figure 5

Particle fractions for the GM1 parameter set for three different values of $z$: (a) $z=0.8$, (b) $z=0.408$ that correspond to the SU(6) case, and (c) $z=0$.

Figure 6

Maximum masses of hyperonic neutron stars as functions of effective nucleon mass $m_N^{*}$ for different values of the $g_8/g_1$ ratio $z$. For comparison, a line for nucleonic stars and points to mark relativistic mean-field sets (e.g., TM1 and NL3) that correspond to the SU(6) case are also given.

Figure 8

The EoS for “model $\sigma \omega \rho \varphi$” in the GM1 parametrization for different values of ${\alpha }_V.z$ is fixed to its SU(6) value $z=1/\sqrt{6}$, and ideal mixing is assumed. The EoS become stiffer with decreasing ${\alpha }_V$.

Figure 9

Mass-radius relations obtained from the EoS in Fig. 8.

Figure 10

Maximum masses of neutron stars as functions of strangeness fraction $f_s$ in the neutron star core for four different parametrizations.