The Structure, Stability, and Dynamics
of Self-Gravitating Systems

Fall Semester, 1997
Project #1

Erik Blaufuss

Energy Transport Processes

Assignment (by J.E. Tohline):

In the current version of this HyperText_Book, I have paid a great deal of attention to the set of equations that govern the equilibrium structure of self-gravitating systems as viewed on a dynamical time scale. Virtually nothing has been said about the need for stars to acquire and maintain a thermodynamical equilibrium in the presence of definite energy losses at their surface. You should present a clear discussion of how energy transport processes are handled in modern models of spherically symmetric stars. Your emphasis should be on the relevant equation(s) that govern radiation transport (by photon random walks!) in stellar interiors (as opposed to stellar atmospheres). Discuss, also, how neutrino transport is handled in models of main-sequence stars and what one must do differently in order to handle neutrino transport in situations (such as supernova explosions) where the cross-section for neutrino interactions becomes relatively large.

The presentation should be in an HTML format and, where possible, a connection should be drawn with the principal governing equations that already have been presented in the book.

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