Editing Apps/RotatingPolytropes/BarmodeLinearTimeDependent (section)

==Index of Relevant Publications==
Here is a list of relevant research papers as largely enumerated by [https://ui.adsabs.harvard.edu/abs/2008PhRvD..78l4001K/abstract Y. Kojima &amp; M. Saijo (2008)] &hellip;

* [TDM85] [https://ui.adsabs.harvard.edu/abs/1985ApJ...298..220T/abstract J. E. Tohline, R. H. Durisen &amp; M. McCollough (1985)], ApJ, 298, 220:  ''The linear and nonlinear dynamic stability of rotating N = 3/2 polytropes''
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<td align="center" width="5%">&nbsp;</td><td align="left">
HYDROCODE:  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 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.
</td></tr></table>

* [DGTB86] [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''
* [WT87] [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''
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<td align="center" width="5%">&nbsp;</td><td align="left">
HYDROCODE:  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.
</td></tr></table>

* [WT88] [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''
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<td align="center" width="5%">&nbsp;</td><td align="left">
Two of the models that were studied in Williams &amp; Tohline (1987) &#8212; specifically, the models having n = 0.8 and 1.8 &#8212; <font color="green">
&hellip; are shown as they evolve to extremely nonlinear amplitudes: the end result in both cases is &hellip; The models shed a fraction of their mass and angular momentum, producing a ring which surrounds a more centrally condensed object &hellip; The central object is a triaxial figure that is rotating about its shortest axis. 
</font><br />
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* [HCS94] [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''
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<td align="center" width="5%">&nbsp;</td><td align="left">
Using Newtonian dynamics and Newtonian gravity <font color="green">&hellip; we have carried out computer simulations of a differentially rotating compact star with a polytropic equation of state undergoing the dynamical bar instability.  This instability has previously been modeled numerically by Tohline and collaborators in the context of star formation &hellip; Our work is the first to calculate</font> [using a post-Newtonian approximation] <font color="green"> the gravitational radiation produced by this instability, including wave forms and luminosities.  It is also a significant advance over the earlier studies because, in addition to using better numerical techniques, we model the fluid correctly using an energy equation.  This is essential due to the generation of entropy by shocks during the later stages of the evolution.
</font><br />

HYDROCODE:  Newtonian, 3D Lagrangian-Cartesian (SPH as implemented by [https://ui.adsabs.harvard.edu/abs/1989ApJS...70..419H/abstract Hernquist &amp; Katz 1989]), Includes energy equation and does ''not'' impose &pi;-symmetry; <math>~\Gamma=5/3</math>; Poisson solved with TREESPH<br />

MODEL(s): Constructed using the SCF method of Smith &amp; Centrella (1992; see article #15 in [https://ui.adsabs.harvard.edu/abs/2005anr..book.....D/abstract R. d'Inverno]), which is based on earlier work of [https://ui.adsabs.harvard.edu/abs/1968ApJ...151.1075O/abstract Ostriker-Mark 1968] and [https://ui.adsabs.harvard.edu/abs/1986ApJS...61..479H/abstract Hachisu 1986]; axisymmetric, n = 3/2 polytrope; n' = 0 rotation law; only one equilibrium configuration, with T/|W| = 0.30.
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* [SHC95] [https://ui.adsabs.harvard.edu/abs/1996ApJ...458..236S/abstract S. C. Smith, J. L. Houser &amp; J. M. Centrella (1995)], ApJ, 458, 236: ''Simulations of Nonaxisymmetric Instability in a Rotating Star: A Comparison between Eulerian and Smooth Particle Hydrodynamics''
* [HC96] [https://ui.adsabs.harvard.edu/abs/1996PhRvD..54.7278H/abstract J. L. Houser &amp; J. M. Centrella (1996)], Phys. Rev. D, 54, 7278:  ''Gravitational radiation from rotational instabilites in compact stellar cores with stiff equations of state''
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<td align="center" width="5%">&nbsp;</td><td align="left">
Extending the work of Houser, Centrella &amp; Smith (1994) just mentioned &#8212; and closely paralleling the work of Williams &amp; Tohline (1987, 1988) &#8212; they examine the development of the dynamical bar instability in configurations that have a range of different equations of state.

HYDROCODE:  Same as Houser, Centrella &amp; Smith (1994) <br />

MODEL(s): Axisymmetric, n' = 0 rotation law; a total of 3 models examined with, respectively,  (n, T/|W|) = (0.5, 0.31), (1.0, 0.32), (1.5, 0.32) &#8212; see their Table II.  The SCF-based method used to construct these models and the (rather contrived) method used to map the continuum distribution of mass into the Lagrangian-based SPH code is discussed in detail in &sect;III of the paper.
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====Break 1====
* [TIPD98] [https://ui.adsabs.harvard.edu/abs/1998ApJ...497..370T/abstract J. Toman, J. N. Imamura, B. J. Pickett &amp; R. H. Durisen (1998)], ApJ, 497, 370:  ''Nonaxisymmetric Dynamic Instabilities of Rotating Polytropes. I. The Kelvin Modes''
<table border="1" align="center" cellpadding="5">
<tr>
  <th align="center" colspan="5">Equilibrium Models constucted and examined by<br />
[https://ui.adsabs.harvard.edu/abs/1998ApJ...497..370T/abstract TIPD98]
 </th>
</tr>
<tr>
  <td align="center"><math>~n</math></td>
  <td align="center"><math>~n'</math></td>
  <td align="center"><math>~T/|W|</math></td>
  <td align="center"><math>~\Omega_p/\Omega_\mathrm{eq}</math></td>
  <td align="center"><math>~R_p/R_\mathrm{eq}</math></td>
</tr>
<tr>
  <td align="center" rowspan=6><math>~\tfrac{5}{4}</math></td>
  <td align="center" rowspan="15">0</td>
  <td align="right">0.274</td>
  <td align="right">2.44</td>
  <td align="left">0.258</td>
</tr>
<tr>
  <td align="right">0.279</td>
  <td align="right">2.45</td>
  <td align="left">0.250</td>
</tr>
<tr>
  <td align="right">0.288</td>
  <td align="right">2.49</td>
  <td align="left">0.234</td>
</tr>
<tr>
  <td align="right">0.319</td>
  <td align="right">2.65</td>
  <td align="left">0.187</td>
</tr>
<tr>
  <td align="right">0.346</td>
  <td align="right">2.88</td>
  <td align="left">0.147</td>
</tr>
<tr>
  <td align="right">0.363</td>
  <td align="right">3.11</td>
  <td align="left">0.123</td>
</tr>
<tr>
  <td align="center" rowspan="16"><math>~\tfrac{3}{2}</math></td>
  <td align="right">0.266</td>
  <td align="right">2.97</td>
  <td align="left">0.258</td>
</tr>
<tr>
  <td align="right">0.280</td>
  <td align="right">3.03</td>
  <td align="left">0.234</td>
</tr>
<tr>
  <td align="right">0.290</td>
  <td align="right">3.09</td>
  <td align="left">0.218</td>
</tr>
<tr>
  <td align="right">0.300</td>
  <td align="right">3.16</td>
  <td align="left">0.202</td>
</tr>
<tr>
  <td align="right">0.316</td>
  <td align="right">3.28</td>
  <td align="left">0.179</td>
</tr>
<tr>
  <td align="right">0.327</td>
  <td align="right">3.35</td>
  <td align="left">0.163</td>
</tr>
<tr>
  <td align="right">0.344</td>
  <td align="right">3.61</td>
  <td align="left">0.139</td>
</tr>
<tr>
  <td align="right">0.368</td>
  <td align="right">4.04</td>
  <td align="left">0.107</td>
</tr>
<tr>
  <td align="right">0.396</td>
  <td align="right">4.79</td>
  <td align="left">0.0754</td>
</tr>
<tr>
  <td align="center" rowspan="4">1</td>
  <td align="right">0.262</td>
  <td align="right">6.85</td>
  <td align="left">0.139</td>
</tr>
<tr>
  <td align="right">0.283</td>
  <td align="right">8.90</td>
  <td align="left">0.107</td>
</tr>
<tr>
  <td align="right">0.292</td>
  <td align="right">9.81</td>
  <td align="left">0.0958</td>
</tr>
<tr>
  <td align="right">0.311</td>
  <td align="right">12.4 &nbsp;</td>
  <td align="left">0.0754</td>
</tr>
<tr>
  <td align="center" rowspan="3"><math>~\tfrac{3}{2}</math></td>
  <td align="right">0.272</td>
  <td align="right">15.1 &nbsp;</td>
  <td align="left">0.0754</td>
</tr>
<tr>
  <td align="right">0.280</td>
  <td align="right">16.9 &nbsp;</td>
  <td align="left">0.0675</td>
</tr>
<tr>
  <td align="right">0.290</td>
  <td align="right">19.0 &nbsp;</td>
  <td align="left">0.0595</td>
</tr>
<tr>
  <td align="center" rowspan="10"><math>~\tfrac{5}{2}</math></td>
  <td align="center" rowspan="10">0</td>
  <td align="right">0.262</td>
  <td align="right">7.19</td>
  <td align="left">0.202</td>
</tr>
<tr>
  <td align="right">0.268</td>
  <td align="right">7.26</td>
  <td align="left">0.194</td>
</tr>
<tr>
  <td align="right">0.273</td>
  <td align="right">7.34</td>
  <td align="left">0.187</td>
</tr>
<tr>
  <td align="right">0.285</td>
  <td align="right">7.52</td>
  <td align="left">0.171</td>
</tr>
<tr>
  <td align="right">0.297</td>
  <td align="right">7.73</td>
  <td align="left">0.155</td>
</tr>
<tr>
  <td align="right">0.304</td>
  <td align="right">7.85</td>
  <td align="left">0.147</td>
</tr>
<tr>
  <td align="right">0.324</td>
  <td align="right">8.29</td>
  <td align="left">0.123</td>
</tr>
<tr>
  <td align="right">0.338</td>
  <td align="right">8.68</td>
  <td align="left">0.107</td>
</tr>
<tr>
  <td align="right">0.371</td>
  <td align="right">9.85</td>
  <td align="left">0.0754</td>
</tr>
<tr>
  <td align="right">0.389</td>
  <td align="right">10.8 &nbsp;</td>
  <td align="left">0.0595</td>
</tr>
</table>

====Break 2====
* [https://ui.adsabs.harvard.edu/abs/2000PhRvD..62f4019N/abstract K. C. B. New, J. M. Centrella &amp; J. E. Tohline (2000)], Phys. Rev. D, 62, 064019:  ''Gravitational waves from long-duration simulations of the dynamical bar instability''
* [https://ui.adsabs.harvard.edu/abs/2000ApJ...542..453S/abstract M. Shibata, T. W. Baumgarte &amp; S. L. Shapiro (2000)], ApJ, 542, 453:  ''The Bar-Mode Instability in Differentially Rotating Neutron Stars: Simulations in Full General Relativity''
* [https://ui.adsabs.harvard.edu/abs/2001MNRAS.324.1063L/abstract Y.-T. Liu &amp; L. Lindblom (2001)], MNRAS, 324, 1063:  ''Models of rapidly rotating neutron stars:  remnants of accretion-induced collapse''
* [https://ui.adsabs.harvard.edu/abs/2001ApJ...548..919S/abstract M. Saijo, M. Shibata, T. W. Baumgarte &amp; S. L. Shapiro (2001)], ApJ, 548, 919: ''Dynamical Bar Instability in Rotating Stars: Effect of General Relativity''
* [https://ui.adsabs.harvard.edu/abs/2001ApJ...550L.193C/abstract J. M. Centrella, K. C. B. New, L. L. Lowe &amp; J. D. Brown (2001)], ApJ, 550, L193: ''Dynamical Rotational Instability at Low T/W''
* [https://ui.adsabs.harvard.edu/abs/2002PhRvD..65l4003L/abstract Y.-T. Liu (2002)], Phys. Rev. D, 65, 124003: ''Dynamical instability of new-born neutron stars as sources of gravitational radiation''
* [https://ui.adsabs.harvard.edu/abs/2003ApJ...595..352S/abstract M. Saijo, T. W. Baumgarte &amp; S. L. Shapiro (2003)], ApJ, 595, 352:  ''One-armed Spiral Instability in Differentially Rotating Stars''
* [https://ui.adsabs.harvard.edu/abs/2006ApJ...651.1068O/abstract S. Ou &amp; J. E. Tohline (2006)], ApJ, 651, 1068:  ''Unexpected Dynamical Instabilities in Differentially Rotating Neutron Stars''
* [https://ui.adsabs.harvard.edu/abs/2007PhRvD..75d4023B/abstract L. Baiotti, R. De Pietri, G. M. Manco &amp; L. Rezzolla (2007)], Phys. Rev. D, 75, 044023: ''Accurate simulations of the dynamical bar-mode instability in full general relativity''
* [https://ui.adsabs.harvard.edu/abs/2007CoPhC.177..288C/abstract P. Cerda-Duran, V. Quilos &amp; J. A. Font (2007)], Comp. Phys. Comm., 177, 288: ''AMR simulations of the low T/|W| bar-mode instability of neutron stars''
* [https://ui.adsabs.harvard.edu/abs/2007ApJ...665.1074O/abstract S. Ou, J. E. Tohline &amp; P. M. Motl (2007)], ApJ, 665, 1074:  ''Further Evidence for an Elliptical Instability in Rotating Fluid Bars and Ellipsoidal Stars''
* [https://ui.adsabs.harvard.edu/abs/2008PhRvD..77f3002S/abstract M. Saijo &amp; Y. Kojima (2008)], Phys. Rev. D, 77, 063002:  ''Faraday resonance in dynamical bar instability of differentially rotating stars''
* [https://ui.adsabs.harvard.edu/abs/2008PhRvD..78l4001K/abstract Y. Kojima &amp; 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'' 
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<td align="center" width="5%">&nbsp;</td><td align="left">
<font color="green">
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;
</font><br />

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''
<table border="0" align="center" width="100%" cellpadding="1"><tr>
<td align="center" width="5%">&nbsp;</td><td align="left">
<font color="green">
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.
</font>
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