AMR simulations of the low T/|W| bar-mode instability of neutron stars

Details AMR simulations of the low T/|W| bar-mode instability of neutron stars AMR simulations of the low T/|W| bar-mode instability of neutron stars

2007-04-03

arxiv.org/abs/0704.0356v1

Comput.Phys.Commun.177:288-297,2007

Astronomy and Astrophysics

Astrophysics

20 pages, 9 figures, accepted for publication in Computer Physics Communications.

Scientific paper

10.1016/j.cpc.2007.04.001

It has been recently argued through numerical work that rotating stars with a high degree of differential rotation are dynamically unstable against bar-mode deformation, even for values of the ratio of rotational kinetic energy to gravitational potential energy as low as O(0.01). This may have implications for gravitational wave astronomy in high-frequency sources such as core collapse supernovae. In this paper we present high-resolution simulations, performed with an adaptive mesh refinement hydrodynamics code, of such low T/|W| bar-mode instability. The complex morphological features involved in the nonlinear dynamics of the instability are revealed in our simulations, which show that the excitation of Kelvin-Helmholtz-like fluid modes outside the corotation radius of the star leads to the saturation of the bar-mode deformation. While the overall trends reported in an earlier investigation are confirmed by our work, we also find that numerical resolution plays an important role during the long-term, nonlinear behaviour of the instability, which has implications on the dynamics of rotating stars and on the attainable amplitudes of the associated gravitational wave signals.

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