Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 334, Issue 2, Pages L27-L31Publisher
OXFORD UNIV PRESS
DOI: 10.1046/j.1365-8711.2002.05724.x
Keywords
gravitational waves; stars : neutron; stars : oscillations; stars : rotation
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We study the dynamical instability against bar-mode deformation of differentially rotating stars. We performed numerical simulation and linear perturbation analysis adopting polytropic equations of state with the polytropic index n= 1. It is found that rotating stars of a high degree of differential rotation are dynamically unstable even for the ratio of the kinetic energy to the gravitational potential energy of O (0.01). Gravitational waves from the final non-axisymmetric quasi-stationary states are calculated in the quadrupole formula. For rotating stars of mass 1.4 M-circle dot and radius several 10 km, gravitational waves have frequency several 100 Hz and effective amplitude similar to5 x 10(-22) at a distance of similar to100 Mpc.
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