Difference between revisions of "User:Tohline/Appendix/Ramblings/MyDoctoralStudents"

From VistrailsWiki
Jump to navigation Jump to search
Line 273: Line 273:
<table border="1" align="center" width="100%" cellpadding="10">
<table border="1" align="center" width="100%" cellpadding="10">
<tr>
<tr>
   <td align="right" rowspan="2" width="10%">1982 - 1988</td>
   <td align="right" rowspan="3" width="10%">1982 - 1988</td>
   <td align="center" bgcolor="lightblue" width="5%">&nbsp;</td>
   <td align="center" bgcolor="lightblue" width="5%">&nbsp;</td>
   <td align="left" width="80%">
   <td align="left" width="80%">
Line 279: Line 279:
Using the HSCF-technique, <font color="red">John Woodward</font> constructed geometrically thick, axisymmetric accretion disk structures having a range of disk-to-central-object mass ratios.  He used CFD techniques to determine which configurations were dynamically stable and which were dynamically unstable toward the development of nonaxisymmetric disk structure.
Using the HSCF-technique, <font color="red">John Woodward</font> constructed geometrically thick, axisymmetric accretion disk structures having a range of disk-to-central-object mass ratios.  He used CFD techniques to determine which configurations were dynamically stable and which were dynamically unstable toward the development of nonaxisymmetric disk structure.
   </td>
   </td>
   <td align="center" rowspan="2">
   <td align="center" rowspan="3">
<b>[</b>[https://ui.adsabs.harvard.edu/abs/1994ApJ...420..247W/abstract 38]<b>]</b><br />
<b>[</b>[https://ui.adsabs.harvard.edu/abs/1994ApJ...420..247W/abstract 38]<b>]</b><br />
<b>[</b>[https://digitalcommons.lsu.edu/gradschool_disstheses/5365/ <math>~\odot</math>]<b>]</b><br />
<b>[</b>[https://digitalcommons.lsu.edu/gradschool_disstheses/5365/ <math>~\odot</math>]<b>]</b><br />
Line 291: Line 291:
   <td align="left">
   <td align="left">
As he was completing his dissertation research, John Woodward took it upon himself to rewrite our 2nd-order-accurate CFD code so that it ran efficiently on the Department of Physics &amp; Astronomy's new, 8K-node SIMD-architecture [https://en.wikipedia.org/wiki/MasPar MasPar computer].  Our 3D, cylindrical-coordinate-based simulations nicely mapped to the MasPar's architecture if we adopted a spatial grid resolution of 64 (in Z) &times; 128 (in R) &#8212; that is, 8K meridional-plane grid zones &#8212; by 128 azimuthal zones "stacked in memory."
As he was completing his dissertation research, John Woodward took it upon himself to rewrite our 2nd-order-accurate CFD code so that it ran efficiently on the Department of Physics &amp; Astronomy's new, 8K-node SIMD-architecture [https://en.wikipedia.org/wiki/MasPar MasPar computer].  Our 3D, cylindrical-coordinate-based simulations nicely mapped to the MasPar's architecture if we adopted a spatial grid resolution of 64 (in Z) &times; 128 (in R) &#8212; that is, 8K meridional-plane grid zones &#8212; by 128 azimuthal zones "stacked in memory."
  </td>
</tr>
<tr>
  <td align="left" bgcolor="pink">&nbsp;</td>
  <td align="left">
Mention 3D imaging using Gabor Herman's software and animation (to VHS) via the NeXT computer.
   </td>
   </td>
</tr>
</tr>

Revision as of 03:50, 1 June 2019

Chronology of Research Endeavors

Whitworth's (1981) Isothermal Free-Energy Surface
|   Tiled Menu   |   Tables of Content   |  Banner Video   |  Tohline Home Page   |

Preface

Looking back, it seems clear to me that the technical book that has had the most influence on my research career has been [EFE], that is, Chandrasekhar's (originally, 1969) Ellipsoidal Figures of Equilibrium. Chandrasekhar evaluated the relative stability of a wide variety of astrophysically interesting (usually Newtonian self-gravitating), rotating equilibrium configurations by employing his own exceptional mathematical skills and those of his students — notably, Norman Lebovitz. When I entered graduate school at UC, Santa Cruz in 1974, [EFE] was the set of glasses through which most astronomers examined stability. Having access to only meager computing resources, Chandrasekhar's descriptions of the onset of instabilities, or evolution between nearly adjacent states, was usually limited to linear-amplitude deviations from equilibrium. From the beginning, I have been interested in using (steadily improving) computational resources to repeat, then extend the analyses found in [EFE] … (1) to configurations with non-homogeneous and compressible structures; and (2) into the nonlinear regime.

The MediaWiki-formatted text that you are reading — titled, The Structure, Stability, & Dynamics of Self-Gravitating Fluids — is my attempt to explain in detail what has been learned as a result of our (and the broader astrophysics community's) extension of the foundation work presented in [EFE]. The chapters of this ever-developing book that, on any date, I consider ready for public consumption can be found on the MediaWiki page that I refer to as the Tiled Menu. The graduate students who have come through my group over the years have made important contributions to the healthy development of this research field. The Outline of Research Activities that is presented, below, highlights and summarizes these contributions.

Doctoral Students Tohline Has Advised

Doctoral Students Whom Tohline has Advised at LSU
Year of Ph.D. Student Name ED Jointly Advised? Quarter-Sized Mosaic Image
1988 Harold Williams <math>~\odot</math>  
1989 Dimitris M. Christodoulou <math>~\odot</math>  
1992 John Woodward <math>~\odot</math>  
1994 Horst Väth <math>~\odot</math> w/ Detlev Koester (Univ. of Kiel, Germany)
1996 Kimberly C. (Barker) New <math>~\odot</math>  
1998 Saied Andalib <math>~\odot</math>  
1998 Erik Young <math>~\odot</math> w/ Ganesh Chanmugam (LSU Physics & Astronomy)
1999 Paul Fisher <math>~\odot</math>  
1999 John E. Cazes <math>~\odot</math>  
1999 Howard S. Cohl <math>~\odot</math>  
2001 Eric I. Barnes <math>~\odot</math>  
2001 Patrick M. Motl <math>~\odot</math> w/ Juhan Frank (LSU Physics & Astronomy)
2004 Shangli Ou <math>~\odot</math>  
2006 Ravi Kumar Kopparapu <math>~\odot</math>  
2006 Richard P. Muffoletto <math>~\odot</math> w/ John Tyler (LSU Computer Science)
2010 Wes P. Even <math>~\odot</math>  
2010 Jay M. Call <math>~\odot</math>  
2011 Dominic C. Marcello <math>~\odot</math>  
2014 Zachary D. Byerly <math>~\odot</math>  

ED = Electronic Dissertation


Annotated

NOTE: In order to see a larger version of the primary image — or its annotated thumbnail companion, shown here, on the right — click once on the image, then click a second time on Full Resolution.


Outline of Research Activities

Here, a brief summary is presented of contributions that we have made toward advancing the astrophysics community's understanding of the structure, stability, & dynamics of self-gravitating fluids. The role that individual LSU graduate students have made to this story has been highlighted. And contributions have each been assigned to one of the following broad categories:

1976 - 1978  

Tohline's dissertation research under the guidance of Peter Bodenheimer (UCSC) and David Black (NASA/Ames Research Center) was an early attempt to examine whether of not isothermal gas clouds whose mass exceeds the Jeans mass spontaneously fragment during a phase of free-fall collapse. The adopted Eulerian computational hydrodynamics scheme was first-order donor-cell based on the 2D (axisymmetric, cylindrical-coordinate) scheme described by Black & Bodenheimer (1976) but extended by Tohline to a 3D grid; a typical simulation was carried out on the CDC 7600 at NASA/Ames and involved 303 ∼ 3 × 104 grid cells.

[PhD]
[4]
[5]
[7]

 

At each integration time step of a simulation, the self-consistently determined, time-dependent Newtonian gravitational potential was determined by combining (1) an FFT technique in the azimuthal coordinate direction, with (2) a Buneman Cyclic Reduction technique in R and Z.

 

Richard Durisen — a NASA/Ames postdoc at the time — said to me something along the lines of, "Hey! When you finish developing that hydrocode, let's get together and examine the dynamical stability of rapidly rotating, equilibrium configurations."

1978 - 1982  

While at Yale University (1978 - 1980) and at Los Alamos National Laboratory (1980 - 1982), Tohline worked closely with Richard Durisen (Indiana University) to examine the onset and nonlinear development of nonaxisymmetric instabilities in differentially rotating, n = 3/2 polytropes whose internal angular momentum distribution was that of an n' = 0 sequence. Generally speaking, unstable eigenfrequencies matched earlier predictions (by other groups) based on linear stability analyses; unstable eigenfunctions displayed a two-armed spiral character. As the amplitude of unstable modes grew to nonlinear amplitude, the developed spiral arms were able to effectively redistribute angular momentum, preventing fragmentation/fission of the configurations. Over this time period, numerical simulations were carried out on the IBM 360/95 at the NASA/Goddard Institute for Space Studies and on an early Cray at Los Alamos.

[16]


[10]
[12]
[13]
[14]


 

Nelson Caldwell — a Yale graduate student at the time — showed Tohline some of his early work focused on the observationally determined properties of elliptical galaxies that display prominent dust lanes. Additional discussions led to a collaboration between Caldwell, Tohline, and Gregory Simonson — also a Yale graduate student at the time — in which the observed orientation of dust lanes can be explained in terms of dissipative settling of gas disks and, as a consequence, can be used to deduce the underlying geometry (e.g., oblate or prolate spheroidal) of each galaxy's mass distribution. With guidance from Tohline, Simonson completed a Yale University doctoral dissertation in which this settling model was extended to the context of polar rings in spiral galaxies.

When Tohline presented a seminar in the Department of Astronomy at Indiana University on the topic of "dust lanes in elliptical galaxies," Durisen asked what would happen to a settling gas disk if the underlying galaxy mass distribution was tumbling end over end — e.g., a cigar spinning about its shortest axis. The ensuing discussions led to a fruitful collaboration between Durisen and Tohline in which it became clear that steady-state warped disks could result. (After Tohline moved to LSU, extensions of this research work resulted in collaborative publications with several LSU graduate students — D. Christodoulou, K. New, H. Väth — and in Paul Fisher's doctoral dissertation research project.)


1982 - 1988  

During his first half-a-dozen years on the faculty at LSU, Tohline continued to worked closely with Richard Durisen (Indiana University) to examine the onset and nonlinear development of nonaxisymmetric instabilities in differentially rotating polytropes. Harold Williams joined this effort as a graduate student in Tohline's group. He broadened the study to include configurations having a range of compressibility and different distributions of angular momentum; this became the central thrust of his doctoral dissertation. Williams also advanced the capabilities of the group's computational tools by implementing a second-order accurate finite-difference scheme to carry out integrations of the governing hydrodynamic equations. Over this time period, numerical simulations were carried out principally on LSU's IBM main-frame computer.

Izumi Hachisu (Kyoto University, Japan) joined the group in a postdoctoral research position for a couple of years. Drawing from his own research background, Hachisu provided us with a blueprint for developing a very efficient numerical algorithm for constructing rapidly rotating equilibrium configurations with spheroidal, toroidal, or binary-star geometric shapes — see our relevant chapter discussion. Over the past several decades, this Hachisu Self-Consistent-Field technique has allowed us to construct a wide range of different self-gravitation configurations as initial states for stability analyses and for examining the nonlinear growth of unstable modes using computational fluid techniques.

[19]
[22]
[<math>~\odot</math>]


[25]
[27]
[33]



[20]

 

A quantitative comparison was made between the results obtained from simulations carried out with two different "finite-difference" computational fluids codes and one "smoothed particle hydrodynamics" algorithm.


1982 - 1988  

Using the HSCF-technique, John Woodward constructed geometrically thick, axisymmetric accretion disk structures having a range of disk-to-central-object mass ratios. He used CFD techniques to determine which configurations were dynamically stable and which were dynamically unstable toward the development of nonaxisymmetric disk structure.

[38]
[<math>~\odot</math>]




 

As he was completing his dissertation research, John Woodward took it upon himself to rewrite our 2nd-order-accurate CFD code so that it ran efficiently on the Department of Physics & Astronomy's new, 8K-node SIMD-architecture MasPar computer. Our 3D, cylindrical-coordinate-based simulations nicely mapped to the MasPar's architecture if we adopted a spatial grid resolution of 64 (in Z) × 128 (in R) — that is, 8K meridional-plane grid zones — by 128 azimuthal zones "stacked in memory."

 

Mention 3D imaging using Gabor Herman's software and animation (to VHS) via the NeXT computer.


Whitworth's (1981) Isothermal Free-Energy Surface

© 2014 - 2021 by Joel E. Tohline
|   H_Book Home   |   YouTube   |
Appendices: | Equations | Variables | References | Ramblings | Images | myphys.lsu | ADS |
Recommended citation:   Tohline, Joel E. (2021), The Structure, Stability, & Dynamics of Self-Gravitating Fluids, a (MediaWiki-based) Vistrails.org publication, https://www.vistrails.org/index.php/User:Tohline/citation