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

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

2009-02-26

arxiv.org/abs/0902.4702v2

Phys.Rev.C80:025801,2009

Physics

Nuclear Physics

Nuclear Theory

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

Scientific paper

10.1103/PhysRevC.80.025801

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 $M/R\geq 0.1078$ independent of the EOS used.

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