User:Tohline/H Book
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Revision as of 09:02, 21 September 2014
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, shortperiod 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>
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Pictorial Table of Contents
Context
 Principal Governing Equations
 Continuity Equation
 Euler Equation
 1^{st} Law of Thermodynamics
 Poisson Equation
Applications
Spherically Symmetric Configurations
Introduction (Alternate Introduction)
Structure:
Solution Strategies: 
Detailed ForceBalance 
Virial Equilibrium 



Stability:
Example Solutions: 
Dynamics:
 Homologously Collapsing Stellar Cores — see, in particular, Goldreich & Weber (1980, ApJ, 238, 991)
TwoDimensional Configurations
 Introduction
Structure:
Solution Strategies 

Example Solutions:

Stability:
Dynamics:
ThreeDimensional Configurations
Structure:
Solution Strategies 
Example Solutions:

Stability:
 Lou & Bai (2011, MNRAS, 415, 925) — 3D perturbations in an isothermal selfsimilar flow
Dynamics:
Related Projects Underway
Appendices
See Also
 NIST Digital Library of Mathematical Functions; see also the related CUP Publication
© 2014  2020 by Joel E. Tohline 