Difference between revisions of "User:Tohline/H Book"

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m (→‎Structure:: Changed "virial analysis" to "virial equilibrium")
(→‎Structure:: Add table structure and link to virial discussion)
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===Structure:===
===Structure:===
 
<table border="1" width="100%" cellspacing="2" cellpadding="8">
* <font color="darkblue">'''Solution Strategies'''</font>
<tr>
** [[User:Tohline/AxisymmetricConfigurations/SolutionStrategies|Axisymmetric Configurations]]
  <td align="left">
 
<font color="darkblue">'''Solution Strategies'''</font>
* Example Solutions:
* [[User:Tohline/AxisymmetricConfigurations/SolutionStrategies|Axisymmetric Configurations]]
** [[User:Tohline/Apps/MaclaurinSpheroids|Maclaurin Spheroids]]
  </td>
** [[User:Tohline/Apps/HayashiNaritaMiyama82|Rotationally Flattened, Isothermal Structures]]
  <td align="right">
** Polytropic Tori:
[[User:Tohline/AxisymmetricConfigurations/Virial|Virial Equilibrium]]
***[[User:Tohline/Apps/PapaloizouPringleTori|Papaloizou-Pringle (massless) Tori]]
  </td>
***Self-gravitating Tori
</tr>
** [[User:Tohline/Apps/Korycansky_Papaloizou_1996|Infinitesimally Thin, Nonaxisymmetric Disk]]
<tr>
  <td align="left" colspan="2">
Example Solutions:
* [[User:Tohline/Apps/MaclaurinSpheroids|Maclaurin Spheroids]]
* [[User:Tohline/Apps/HayashiNaritaMiyama82|Rotationally Flattened, Isothermal Structures]]
* Polytropic Tori:
**[[User:Tohline/Apps/PapaloizouPringleTori|Papaloizou-Pringle (massless) Tori]]
**Self-gravitating Tori
* [[User:Tohline/Apps/Korycansky_Papaloizou_1996|Infinitesimally Thin, Nonaxisymmetric Disk]]
  </td>
</tr>
</table>


===Stability:===
===Stability:===

Revision as of 21:34, 9 September 2012


Whitworth's (1981) Isothermal Free-Energy Surface
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Preface from the original version of this HyperText Book (H_Book):

November 18, 1994

Much of our present, basic understanding of the structure, stability, and dynamical evolution of individual stars, short-period binary star systems, and the gaseous disks that are associated with numerous types of stellar systems (including galaxies) is derived from an examination of the behavior of a specific set of coupled, partial differential equations. These equations — most of which also are heavily utilized in studies of continuum flows in terrestrial environments — are thought to govern the underlying physics of all macroscopic "fluid" systems in astronomy. Although relatively simple in form, they prove to be very rich in nature... <more>

Pictorial Table of Contents

Context

  • Virial Equations

Applications

Spherically Symmetric Configurations

Introduction

Structure:

Solution Strategies

Virial Equilibrium

Example Solutions:

Stability:

Solution Strategy

Virial Stability

Example Solutions:

Dynamics:

Two-Dimensional Configurations

Structure:

Solution Strategies

Virial Equilibrium

Example Solutions:

Stability:

Dynamics:

Three-Dimensional Configurations

Structure:

Stability:

Dynamics:

Appendices


See Also


Whitworth's (1981) Isothermal Free-Energy Surface

© 2014 - 2021 by Joel E. Tohline
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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