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

Abstract

The eigen-frequencies 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 eigen-frequencies 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 $M/R\ge 0.1078$ independent of the EOS used.

Version appeared in Phys. Rev. C80, 025801 (2009)

References in corpus (3)

• Neutron Star Observations: Prognosis for Equation of State Constraints
• Nuclear symmetry energy probed by neutron skin thickness of nuclei
• Isoscaling as a measure of Symmetry Energy in the Lattice Gas Model

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• Energy release from hadron-quark phase transition in neutron stars and the axial $w$-mode of gravitational waves
• Dependence of relative abundances of constituents in dense stellar matter on nuclear symmetry energy