Neutron Star instabilities in full General Relativity using a ideal fluid
arXiv:1403.8066 · doi:10.1103/PhysRevD.90.024034
Abstract
We present results about the effect of the use of a stiffer equation of state, namely the ideal-fluid ones, on the dynamical bar-mode instability in rapidly rotating polytropic models of neutron stars in full General Relativity. We determine the change on the critical value of the instability parameter for the emergence of the instability when the adiabatic index is changed from 2 to 2.75 in order to mimic the behavior of a realistic equation of state. In particular, we show that the threshold for the onset of the bar-mode instability is reduced by this change in the stiffness and give a precise quantification of the change in value of the critical parameter . We also extend the analysis to lower values of and show that low-beta shear instabilities are present also in the case of matter described by a simple polytropic equation of state.
16 pages, 16 figures
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