An equation of state for warm neutron degenerate matter

Details An equation of state for warm neutron degenerate matter An equation of state for warm neutron degenerate matter

Aug 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979mnras.188..565l&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Vol. 188, p. 565-578 (1979)

Astronomy and Astrophysics

Astronomy

4

Scientific paper

The equation of state of Langer et al. is extended to non-zero temperatures. The gas is considered to be an equilibrium mixture of degenerate neutrons, protons, electrons, positrons, negative muons and a single species of nucleus. The pressure and equilibrium particle concentrations are tabulated for densities and temperatures which may occur at the centre of a pre-supernova during gravitational collapse (2 × 1011 < ρ < 1016 g cm-3; 1010 < T < 4.5 × l011 K.
The results agree (to within a factor of 2) with the equation of state derived by El Eid & Hilf except at high densities or high temperatures.

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