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Revision as of 14:09, 23 April 2010
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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
- Principal Governing Equations
- Continuity Equation
- Euler Equation
- <math>1^\mathrm{st}</math> Law of Thermodynamics
- Poisson Equation
- Virial Equations
Applications
Spherically Symmetric Configurations
Structure:
- Solution Strategies
- Example Solutions:
- Uniform-density sphere
- Polytropes
- Power-law density distribution
- Zero-temperature White Dwarf
- Isothermal sphere
Stability:
- Solution Strategy
- Example Solutions:
Dynamics:
Two-Dimensional Configurations
- Introduction
Structure:
- Solution Strategies
- Example Solutions:
Stability:
Dynamics:
Three-Dimensional Configurations
- Introduction
Structure:
- Solution Strategies
- Example Solutions:
- Ellipsoidal Figures of Equilibrium
- Compressible Analogs of Riemann Ellipsoids
Stability:
Dynamics:
Appendices
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© 2014 - 2021 by Joel E. Tohline |