Editing Apps/RotatingPolytropes/BarmodeLinearTimeDependent (section)

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Nonlinear growth of the bar-mode deformation is studied for a differentially rotating star with supercritical rotational energy. In particular, the growth mechanism of some azimuthal modes with odd wave numbers is examined &hellip; Mode coupling to even modes, i.e., the bar mode and higher harmonics, significantly enhances the amplitudes of odd modes &hellip;
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HYDROCODE:  Newtonian, 3D Eulerian, Cartesian, with entropy tracer; reflection symmetry through equatorial plane; <math>~\Gamma=2</math>; Poisson solved with preconditioned conjugate gradient (PCG) method<br />

MODEL(s):  axisymmetric, n = 1 polytrope; [[AxisymmetricConfigurations/SolutionStrategies#SRPtable|j-constant rotation law]] with A = 1; their Table I lists four different equilibrium configurations having T/|W| = 0.256, 0.268, 0.277, 0.281.
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Additional references identified through the above set of references:
* [https://ui.adsabs.harvard.edu/abs/2018PhRvD..98b4003S/abstract M. Saijo (2018)], Phys. Rev. D, 98, 024003:  ''Determining the stiffness of the equation of state using low T/W dynamical instabilities in differentially rotating stars''
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We investigate the nature of low T/W dynamical instabilities in various ranges of the stiffness of the equation of state in differentially rotating stars &hellip; We analyze these instabilities in both a linear perturbation analysis and a three-dimensional hydrodynamical simulation &hellip; the nature of the eigenfunction that oscillates between corotation and the surface for an unstable star requires reinterpretation of pulsation modes in differentially rotating stars.
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