Neutrino flow and gravitational collapse Page: 6 of 37
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Fe = gHe = log (2.5 x 10-12p)-(p - 4 x 1011)/p; P> 4 x 1011 g/cm3
(4) gb = 0,
gFe = gHe = gb = 0; P< 4 x 1011 g/cm3.
Nuclear atomic weights are approximated by
A = 56. x expE(P1/3-400.)l.35 x 10~4]; p> 6.4 x 10 g/cm3,
(5) A = 56; P< 6.4 x 10 g/cm
eq = Ae
Ae x 4j56 .
The deviations of the actual A and 2 from the equilibrium values Aeq and
Zeq are calculated as part of the neutrino flow. In stellar collapse, the
neutron drip-point may be strongly shifted relative to zero neutrino number
calculations because the core is many neutrino mean free paths across and
contains a high neutrino chemical potential. 14 Our calculations neglect this
effect and so overestimate the pressure; however, the final bounce density is
so high that the neutrons surely "dripped" most of the nuclei at the bounce.
The free energy F is minimized with respect to X to find the X.. Heavy
particle pressure and energy are then computed from the thermodynamic relations
2 SF 2 _(/T)
P - P - and e = -T2 a(F/T)
nuc 3P nut 3T
to this pressure and energy is added the electron pressure
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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/m1/6/: accessed February 18, 2019), University of North Texas Libraries, Digital Library, digital.library.unt.edu; crediting UNT Libraries Government Documents Department.