A mean-field calculation of the equation of state of supernova matter

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The equation of state for hot dense matter occurring in stellar collapse is calculated using the Hartree-Fock approximation at finite temperature. The effective nucleon-nucleon interaction is a modified Skyrme force which gives a rather good value of the compression modulus in nuclear matter. Results are presented for the adiabat S = 1 per baryon, with a fixed value of the electron fraction Ye = 0.25, in the density range ρ = 0.02 to 0.07 baryons per fm3. We find that nuclei are still present in the medium. As a consequence the adiabatic index is slightly less than 4 3. We also discuss the presence of a transition, around half nuclear matter density, towards a phase made of bubbles. © 1981.




Bonche, P., & Vautherin, D. (1981). A mean-field calculation of the equation of state of supernova matter. Nuclear Physics, Section A, 372(3), 496–526. https://doi.org/10.1016/0375-9474(81)90049-X

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