Stiffness effects on the dynamics of the bar-mode instability of Neutron Stars in full General Relativity

Abstract

We present results on the effect of the stiffness of the equation of state on the dynamical bar-mode instability in rapidly rotating polytropic models of neutron stars in full General Relativity. We determine the change in the threshold for the emergence of the instability for a range of the adiabatic $\Gamma$ index from 2.0 to 3.0, including two values chosen to mimic more realistic equations of state at high densities.

12 pages, 5 figures. arXiv admin note: substantial text overlap with arXiv:1403.8066

References in corpus (4)

• Relativistic neutron star merger simulations with non-zero temperature equations of state I. Variation of binary parameters and equation of state
• Accurate simulations of the dynamical bar-mode instability in full General Relativity
• Dynamical non-axisymmetric instabilities in rotating relativistic stars
• Non-axisymmetric instability and fragmentation of general relativistic quasi-toroidal stars

Cited by in corpus (4)

• Modeling differential rotations of compact stars in equilibriums
• Modeling Mergers of Known Galactic Systems of Binary Neutron Stars
• Evolution of bare quark stars in full general relativity: Single star case
• Impact of ultralight bosonic dark matter on the dynamical bar-mode instability of rotating neutron stars