Effect of the DDM3Y Nuclear Equation of State on the R-mode Instability of Neutron Stars

Abstract

The r-mode instability windows of neutron stars in the slow rotation approximation are explored using the equation of state obtained from the density dependent M3Y effective interaction. We consider the neutron star matter to be β-equilibrated neutron-proton-electron matter at the core with a rigid crust. The critical frequencies as functions of temperature are calculated for a wide range of neutron star masses. We conclude that the young and hot rotating neutron stars lie in the r-mode instability region. We also stress on the fact that if the dominant dissipative mechanism of the r-mode is the shear viscosity along the boundary layer of the crust-core interface, then the neutron stars with low value of slope of symmetry energy L lie in the r-mode instability region and hence emit gravitational radiation.