Difference between revisions of "User:Tohline/H Book"
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short-period binary star systems, and the gaseous disks that are associated | short-period binary star systems, and the gaseous disks that are associated | ||
with numerous types of stellar systems (including galaxies) is derived | 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 | 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... [http://www.vistrails.org/index.php/User:Tohline/Preface <more>] | ||
govern the underlying physics of all macroscopic "fluid" systems in | |||
astronomy. Although relatively simple in form, they prove to be very rich | |||
in nature... [http://www.vistrails.org/index.php/User:Tohline/Preface <more>] | |||
==Context== | ==Context== | ||
Revision as of 18:16, 18 January 2010
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
- Supplemental Relations
- Virial Equations
Applications
Structure
Stability
Dynamics
