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

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==Applications==
==Applications==


# <font color="darkblue">'''Non-rotating, uniform-density sphere:'''</font>
# <font color="darkblue">'''[http://www.vistrails.org/index.php/User:Tohline/SphericallySymmetricStructures Spherically Symmetric Structures]:'''</font>
 
 
<div align="right">
<table border=1 cellpadding=8 width="95%">
<tr>
  <td width="10%" align="center" valign="top">
Structure<br />
[[Image:LSU_Structure_still.gif|74px]]
  </td>
  <td align="left" valign="top">
<font color="red">SUMMARY:</font> The equilibrium structure of a self-gravitating, non-rotating, uniform-density sphere can be described analytically.  The equilibrium structure of a self-gravitating, non-rotating, uniform-density sphere can be described analytically.  The equilibrium structure of a self-gravitating, non-rotating, uniform-density sphere can be described analytically.  The equilibrium structure of a self-gravitating, non-rotating, uniform-density sphere can be described analytically.  The equilibrium structure of a self-gravitating, non-rotating, uniform-density sphere can be described analytically.  The equilibrium structure of a self-gravitating, non-rotating, uniform-density sphere can be described analytically. The equilibrium structure of a self-gravitating, non-rotating, uniform-density sphere can be described analytically.
  </td>
</tr>
 
<tr>
  <td width="10%" align="center" valign="top">
Stability<br />
[[Image:LSU_Stable.animated.gif|74px]]
  </td>
  <td align="left" valign="top">
<font color="red">SUMMARY:</font> The equilibrium structure of a self-gravitating, non-rotating, uniform-density sphere can be described analytically.  The equilibrium structure of a self-gravitating, non-rotating, uniform-density sphere can be described analytically.  The equilibrium structure of a self-gravitating, non-rotating, uniform-density sphere can be described analytically.  The equilibrium structure of a self-gravitating, non-rotating, uniform-density sphere can be described analytically.  The equilibrium structure of a self-gravitating, non-rotating, uniform-density sphere can be described analytically.  The equilibrium structure of a self-gravitating, non-rotating, uniform-density sphere can be described analytically.  The equilibrium structure of a self-gravitating, non-rotating, uniform-density sphere can be described analytically.
  </td>
</tr>
 
<tr>
  <td width="10%" align="center" valign="top">
Dynamics<br />
[[Image:Minitorus.animated.gif|74px]]
  </td>
  <td align="left" valign="top">
<font color="red">SUMMARY:</font> The equilibrium structure of a self-gravitating, non-rotating, uniform-density sphere can be described analytically.  The equilibrium structure of a self-gravitating, non-rotating, uniform-density sphere can be described analytically.  The equilibrium structure of a self-gravitating, non-rotating, uniform-density sphere can be described analytically.  The equilibrium structure of a self-gravitating, non-rotating, uniform-density sphere can be described analytically.  The equilibrium structure of a self-gravitating, non-rotating, uniform-density sphere can be described analytically.  The equilibrium structure of a self-gravitating, non-rotating, uniform-density sphere can be described analytically.  The equilibrium structure of a self-gravitating, non-rotating, uniform-density sphere can be described analytically.
  </td>
</tr>
 
</table>
</div>


==Appendices==
==Appendices==


{{LSU_HBook_footer}}
{{LSU_HBook_footer}}

Revision as of 21:33, 31 January 2010


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>

Context

Principal Governing Equations
Supplemental Relations
Virial Equations

Applications

  1. Spherically Symmetric Structures:

Appendices

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