Editing Appendix/Ramblings/MyDoctoralStudents (section)

===Years 2000 - 2005===
<!-- 2000 - 2005 -->
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  <td align="center">[http://www.phys.lsu.edu/~tohline/ref_ref.html Pubs.] <font color="red">(rank)</font></td>
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In collaboration with [http://www.ccom.ucsd.edu/~lindblom/ Lee Lindblom] (Caltech) and Tohline, <font color="red">Shangli Ou</font> simulated the secular development of the so-called ''Dedekind bar-mode instability'' in rapidly rotating, initially axisymmetric polytropes.  The numerical simulations were carried out using the MPI-based version of LSU's CFD code &#8212; developed by LSU graduate student, <font color="red">Patrick Motl</font> &#8212; modified to include a physically relevant post-Newtonian driving term.

With guidance from Tohline, Ou also used the group's MPI-based CFD code &#8212; without post-Newtonian driving terms &#8212; to simulate the development of:  (1) a one-armed spiral instability in low-T/|W| postbounce supernova cores (in collaboration with Christian D. Ott and Adam Burrows); (2) an unexpected dynamical instability in differentially rotating neutron stars; and (3) an elliptical instability in rotating fluid bars and ellipsoidal stars (in collaboration with Patrick Motl).
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<b>[</b>[https://digitalcommons.lsu.edu/gradschool_dissertations/4005/ <math>~\odot</math>]<b>]</b><br />
<b>[</b>[https://ui.adsabs.harvard.edu/abs/2004ApJ...617..490O/abstract 65]<b>]</b><br />
<b>[</b>[https://ui.adsabs.harvard.edu/abs/2005ApJ...625L.119O/abstract 66]<b>]</b> <font color="red">(10<sup>th</sup>)</font><br />
<b>[</b>[https://ui.adsabs.harvard.edu/abs/2006ApJ...651.1068O/abstract 68]<b>]</b><br />
<b>[</b>[https://ui.adsabs.harvard.edu/abs/2007ApJ...665.1074O/abstract 70]<b>]</b><br />
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<b>[</b>[https://digitalcommons.lsu.edu/gradschool_disstheses/263/ <math>~\odot</math>]<b>]</b><br />
<b>[</b>[https://ui.adsabs.harvard.edu/abs/2001ApJ...551...80B/abstract 58]<b>]</b><br />
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<b>[</b>[https://digitalcommons.lsu.edu/gradschool_dissertations/2565/ <math>~\odot</math>]<b>]</b><br />
<b>[</b>[https://ui.adsabs.harvard.edu/abs/2002ApJS..138..121M/abstract 61]<b>]</b><br />
<b>[</b>[https://ui.adsabs.harvard.edu/abs/2006ApJ...643..381D/abstract 67]<b>]</b> <font color="red">(11<sup>th</sup>)</font><br />
<b>[</b>[https://ui.adsabs.harvard.edu/abs/2007ApJ...670.1314M/abstract 71]<b>]</b> <font color="red">(18<sup>th</sup>)</font><br />
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Suppose the ''compressible analog of a Riemann ellipsoid'' that developed  during one of Cazes' simulations (see above, under Years 1994 - 2000) is scaled up in size to represent a dynamically stable, spinning gaseous bar at the center of a (barred) spiral galaxy.  Individual stars that form from this gaseous bar will be ''injected'' into the galaxy with a velocity vector that corresponds to the velocity vector that the gas has ''at the location where the star formed.''  But because the "point-like" star will not be influenced by the gas pressure after its formation, the star must follow a trajectory that is different from the gas streamlines.  Using n-body simulations, <font color="red">Eric I. Barnes</font> identified the families of stellar orbits that become occupied by stars that are formed from such steady-state bars.
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With [https://www.lsu.edu/physics/people/faculty/frank.php Juhan Frank] as his primary doctoral advisor and Tohline as secondary advisor, <font color="red">Patrick M. Motl</font> made significant improvements to the group's CFD code (see above, under [[#Years_1994_-_2000|Years 1994 - 2000)]] and used the code to simulate mass-transfer in unequal-mass, semi-detached binary systems.  Both stars had polytropic equations of state but, otherwise, the initially synchronously rotating model configurations were chosen to represent white dwarf pairs.  Numerous evolutions were followed from the onset of mass transfer to (i) merger, (ii) tidal disruption, or (iii) detachment.
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