|Author||Epstein, R. I. ♦ Arnett, W. D.|
|Source||United States Department of Energy Office of Scientific and Technical Information|
|Publisher||Institute of Physics (IOP)|
|Subject Keyword||Physics (Astrophysics & Cosmology)-Stars ♦ Physics Research-Astrophysics & Cosmology-Stars ♦ STAR EVOLUTION- NUCLEAR REACTIONS ♦ COSMOCHEMISTRY ♦ DENSITY ♦ EQUATIONS OF STATE ♦ HYDROGEN ♦ MATTER ♦ NEUTRONS ♦ STARS|
|Abstract||The properties of matter in nuclear statistical equilibrium are investigated over the range of density, temperature, and electron number 10$sup 9$approximately-less-thanrhoapproximately-less-than10$sup 11$ g cm$sup -3$, 2times10$sup 9$approximately-less-thanTapproximately-less-than4times10$sup 10$, and 0.50approximately-less-thanY/sube/approximately-less-than0.45; it is just this range of parameters which is relevant for stellar material subsequent to silicon burning. The ion number, the nuclear binding energy, and the rates of neutronization and energy emission by neutrinos have been calculated. The present results are compared with those of previous workers, and their accuracy is critically assessed. A simple phenomenological picture of the relevant physical processes is presented and is used to develop approximate expressions for the weak interaction rates and the thermodynamic properties of the matter. The approximate results are presented in a form which is suitable for numerical investigations. (AIP)|
|Learning Resource Type||Article|
|Publisher Department||Center for Astrophysics, Harvard College Observatory and Smithsonian Astrophysical Observatory, Cambridge, MA|
|Publisher Place||United States|
|Organization||Center for Astrophysics, Harvard College Observatory and Smithsonian Astrophysical Observatory, Cambridge, MA|
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