Neutrino flow and gravitational collapse Page: 4 of 37
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the explosion was narginally dependent on the details of the neutrino
interactions, and the calculational model had several weaknesses. The present
work was undertaken to clarify the situation. In particular, the calculations
described here include the explicit calculation of all four neutrino types and
treat both electron and neutrino degeneracy.
DETAILS OF MODEL
Equation of State
The models we consider begin with a star in the mass range (Arnett 3) of
8-30M0 at the end of its thermonuclear burning, that is burning quietly to Fe.
When the Fe core has grown to about 1.5M0, the central pressure and temperature
are sufficiently high for the Fe to decompose and absorb electrons. This
initiates the collapse of the star. The core starts collapsing at a central
density of about 109 g/cm3and at a temperature of about 0.5 MeV. The core then
collapses to a density of about 1014 g/cm3and to a temperature of 10 MeV. The
outside of the Fe core has a density of about 106 to 107 g/cm , temperatures of
a few hundred kilovolts, and is almost nondegenerace. This is the principal
region of concern for the equation c' state.
The stellar material is considered to be made of heavy nuclei representing
the Fe group of elements, He, protons. neutrons, and electrons. First, we
write a free energy for the heavy particles:
( I F1 ) _____
(1) F = i( (-T + -i(log 5/2 3/2 +
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Wilson, J.R. Neutrino flow and gravitational collapse, article, August 18, 1975; Livermore, California. (digital.library.unt.edu/ark:/67531/metadc872174/m1/4/: accessed November 21, 2018), University of North Texas Libraries, Digital Library, digital.library.unt.edu; crediting UNT Libraries Government Documents Department.