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Tsuruta, S., and A.G.W. Cameron, 1965: Composition of matter in nuclear statistical equilibrium at high densities. Can. J. Phys., 43, 2056-2077, doi:10.1139/p65-199.
Various properties of dense matter in nuclear statistical equilibrium are studied for densities and temperatures in the range 106 ≤ ρ $lt;= 1012 g/cm3 and 2*times$109 ≤ T $lt;= 1010°K. With increasing density the stability shifts to more and more neutron-rich nuclei. With increasing temperature the general tendency is that nuclei of smaller charge become more abundant, and the abundances of nuclei near a peak tend to become nearly as large as that of the peak nucleus. The shifting of the most stable region with change of density or temperature takes place rather abruptly from one neutron closed shell region to the next. For densities ≤ ~ 106 g/cm3, the ordinary iron group nuclei are most stable until the temperature becomes about 5×109°K; for higher temperatures matter in equilibrium consists of almost pure helium. For higher density, this transition to a helium phase takes place at a somewhat higher temperature, and the equilibrium configuration for temperatures below the helium transition point shifts to the neutron-rich side of the valley of beta stability. When , matter consists of almost pure neutrons at all densities. Rates of beta reactions and neutrino emission generally increase with increase of density and temperature. At a typical temperature of about 5×109°°K, the neutrino energy emission rate increases from about 2×1011 ergs/g sec at ρ ~ 106 g/cm3 to about 2×1017 erg/g sec at ρ ~ 3×1011 g/cm3.
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