Difference between revisions of "User:Tohline/Apps/RotatingPolytropes/BarmodeLinearTimeDependent"

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CODE:  Newtonian, 3D Eulerian, cylindrical; &pi;-symmetry plus reflection symmetry through equatorial plane; <math>~\Gamma=5/3</math>; Poisson solved with FFT + Buneman cyclic reduction<br />
CODE:  Newtonian, 3D Eulerian, 1<sup>st</sup>-order donor-cell on a cylindrical grid; &pi;-symmetry plus reflection symmetry through equatorial plane; <math>~\Gamma=5/3</math>; Poisson solved with FFT + Buneman cyclic reduction<br />


MODEL(s): Constructed using Striker-Mark SCF method; axisymmetric, n = 3/2 polytrope; n' = 0 rotation law; four different equilibrium configurations having T/|W| = 0.28, 0.30, 0.33, 0.35.
MODEL(s): Constructed using Ostriker-Mark SCF method; axisymmetric, n = 3/2 polytrope; n' = 0 rotation law; four different equilibrium configurations having T/|W| = 0.28, 0.30, 0.33, 0.35.
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* [https://ui.adsabs.harvard.edu/abs/1986ApJ...305..281D/abstract R. H. Durisen, R. A. Gingold, J. E. Tohline &amp; A. P. Boss (1986)], ApJ, 305, 281: ''Dynamic Fission Instabilities in Rapidly Rotating N = 3/2 Polytropes: A Comparison of Results from Finite-Difference and Smoothed Particle Hydrodynamics Codes''
* [https://ui.adsabs.harvard.edu/abs/1986ApJ...305..281D/abstract R. H. Durisen, R. A. Gingold, J. E. Tohline &amp; A. P. Boss (1986)], ApJ, 305, 281: ''Dynamic Fission Instabilities in Rapidly Rotating N = 3/2 Polytropes: A Comparison of Results from Finite-Difference and Smoothed Particle Hydrodynamics Codes''
* [https://ui.adsabs.harvard.edu/abs/1987ApJ...315..594W/abstract H. A. Williams &amp; J. E. Tohline (1987)], ApJ, 315, 594:  ''Linear and Nonlinear Dynamic Instability of Rotating Polytropes''
* [https://ui.adsabs.harvard.edu/abs/1987ApJ...315..594W/abstract H. A. Williams &amp; J. E. Tohline (1987)], ApJ, 315, 594:  ''Linear and Nonlinear Dynamic Instability of Rotating Polytropes''
<table border="0" align="center" width="100%" cellpadding="1"><tr>
<td align="center" width="5%">&nbsp;</td><td align="left">
CODE:  Same as in [https://ui.adsabs.harvard.edu/abs/1985ApJ...298..220T/abstract Tohline, Durisen &amp; McCollough (1985)], above.<br />
MODEL(s): Constructed using Ostriker-Mark SCF method; axisymmetric, n' = 0 rotation law; five different equilibrium configurations having (see column 1 of their Table 1) n = 0.8, 1.0, 1.3, 1.5, 1.8, all having T/|W| = 0.310.
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* [https://ui.adsabs.harvard.edu/abs/1988ApJ...334..449W/abstract H. A. Williams &amp; J. E. Tohline (1988)], ApJ, 334, 449:  ''Circumstellar Ring Formation in Rapidly Rotating Protostars''
* [https://ui.adsabs.harvard.edu/abs/1988ApJ...334..449W/abstract H. A. Williams &amp; J. E. Tohline (1988)], ApJ, 334, 449:  ''Circumstellar Ring Formation in Rapidly Rotating Protostars''
* [https://ui.adsabs.harvard.edu/abs/1994PhRvL..72.1314H/abstract J. L. Houser, J. M. Centrella &amp; S. C. Smith (1994)], PRL, 72, 1314: ''Gravitational radiation from nonaxisymmetric instability in a rotating star''
* [https://ui.adsabs.harvard.edu/abs/1994PhRvL..72.1314H/abstract J. L. Houser, J. M. Centrella &amp; S. C. Smith (1994)], PRL, 72, 1314: ''Gravitational radiation from nonaxisymmetric instability in a rotating star''

Revision as of 03:50, 2 July 2019

Simulating the Onset of a Barmode Instability

Whitworth's (1981) Isothermal Free-Energy Surface
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Index of Relevant Publications

Here is a list of relevant research papers as enumerated by …

  • Y. Kojima & M. Saijo (2008), Phys. Rev. D, vol. 78, Issue 12, id. 124001: Amplification of azimuthal modes with odd wave numbers during dynamical bar-mode growth in rotating stars
 

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 … Mode coupling to even modes, i.e., the bar mode and higher harmonics, significantly enhances the amplitudes of odd modes …

CODE: Newtonian, 3D Eulerian, Cartesian, with entropy tracer; reflection symmetry through equatorial plane; <math>~\Gamma=2</math>; Poisson solved with preconditioned conjugate gradient (PCG) method

MODEL(s): axisymmetric, n = 1 polytrope; 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.

 

CODE: Newtonian, 3D Eulerian, 1st-order donor-cell on a cylindrical grid; π-symmetry plus reflection symmetry through equatorial plane; <math>~\Gamma=5/3</math>; Poisson solved with FFT + Buneman cyclic reduction

MODEL(s): Constructed using Ostriker-Mark SCF method; axisymmetric, n = 3/2 polytrope; n' = 0 rotation law; four different equilibrium configurations having T/|W| = 0.28, 0.30, 0.33, 0.35.

 

CODE: Same as in Tohline, Durisen & McCollough (1985), above.

MODEL(s): Constructed using Ostriker-Mark SCF method; axisymmetric, n' = 0 rotation law; five different equilibrium configurations having (see column 1 of their Table 1) n = 0.8, 1.0, 1.3, 1.5, 1.8, all having T/|W| = 0.310.

Additional references identified through the above set of references:

  • 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
 

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 … We analyze these instabilities in both a linear perturbation analysis and a three-dimensional hydrodynamical simulation … 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.

See Also


Whitworth's (1981) Isothermal Free-Energy Surface

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