Imprints of the nuclear symmetry energy on gravitational waves from the axial w-modes of neutron stars

The eigenfrequencies of the axial w-modes of oscillating neutron stars are studied using the continued fraction method with an equation of state (EOS) partially constrained by the recent terrestrial nuclear laboratory data. It is shown that the density dependence of the nuclear symmetry energy E-sym(rho) affects significantly both the frequencies and the damping times of these modes. Besides confirming the previously found universal behavior of the mass-scaled eigenfrequencies as functions of the compactness of neutron stars, we explored several alternative universal scaling functions. Moreover, the w(II)-mode is found to exist only for neutron stars having a compactness of M/R >= 0.1078 independent of the EOS used.