1205.4897 (Ch. C. Moustakidis)

Nuclear Equation of State Effects on r-modes Instabilities in Neutron Stars    [PDF]

Ch. C. Moustakidis

We study the effect of nuclear equation of state on the r-mode instability of a rotating neutron star. We consider the case where the crust of the neutron star is perfectly rigid and we employ the related theory introduced by Lindblom {\it et al.} \cite{Lidblom-2000}. The gravitational and the viscous time scales, the critical angular velocity and the critical temperature are evaluated by employing a phenomenological nuclear model for the neutron star matter. The predicted equations of state for the $\beta$-stable nuclear matter are parameterized by varying the slope $L$ of the symmetry energy at saturation density on the interval $50 \ {\rm MeV} \leq L \leq 110 \ {\rm MeV}$. The effects of the density dependence of the nuclear symmetry energy on r-mode instability properties are presented and analyzed. A comparison of theoretical predictions with observed neutron stars in low-mass x-ray binaries is also performed and analyzed.

View original: http://arxiv.org/abs/1205.4897