Hyperon bulk viscosity and r-modes of neutron stars

We propose and apply a new parametrization of the modified chiral effective model to study rotating neutron stars with hyperon cores in the framework of the relativistic mean-field theory. The inclusion of mesonic cross couplings in the model has improved the density content of the symmetry energy slope parameters, which are in agreement with the findings from recent terrestrial experiments. The bulk viscosity of the hyperonic medium is analyzed to investigate its role in the suppression of gravitationally driven r-modes. The hyperonic bulk viscosity coefficient caused by non-leptonic weak interactions and the corresponding damping time-scales are calculated and the r-mode instability windows are obtained. The present model predicts a significant reduction of the unstable region due to a more effective damping of oscillations. We find that from similar to 10(8) K to similar to 10(9) K, hyperonic bulk viscosity completely suppresses the r-modes leading to a stable region between the instability windows. Our analysis indicates that the instability can reduce the angular velocity of the star up to similar to 0.3 omega(K), where omega(K) is the Kepler frequency of the star.

Automated summary

We propose and apply a new parametrization of the modified chiral effective model to study rotating neutron stars with hyperon cores. The inclusion of mesonic cross couplings in the model has improved the density content of the symmetry energy slope parameters. The analysis of the hyperonic bulk viscosity shows that it completely suppresses the gravitationally driven r-modes, leading to a stable region between the instability windows.