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
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.