Equation of State of Dense Matter from a density dependent relativistic mean field model

Abstract

We calculate the equation of state (EoS) of dense matter, using a relativistic mean field (RMF) model with a density dependent coupling that is a slightly modified form of the original NL3 interaction. For nonuniform nuclear matter we approximate the unit lattice as a spherical Wigner-Seitz cell, wherein the meson mean fields and nucleon Dirac wave functions are solved fully self-consistently. We also calculate uniform nuclear matter for a wide range of temperatures, densities, and proton fractions, and match them to non-uniform matter as the density decreases. The calculations took over 6,000 CPU days in Indiana University's supercomputer clusters. We tabulate the resulting EoS at over 107,000 grid points in the proton fraction range $Y_P$ = 0 to 0.56. For the temperature range $T$ = 0.16 to 15.8 MeV we cover the density range $n_B$ = 10${}^{-4}$ to 1.6 fm${}^{-3}$; and for the higher temperature range $T$ = 15.8 to 80 MeV we cover the larger density range $n_B$ = 10${}^{-8}$ to 1.6 fm${}^{-3}$. In the future we plan to study low density, low temperature (T$<$15.8 MeV), nuclear matter using a Virial expansion, and we will match the low density and high density results to generate a complete EoS table for use in astrophysical simulations of supernova and neutron star mergers.

Modified introduction. Add discussions on other equation of state. 12 pages, 6 figures, Phys. Rev. C in press

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• Neutron-Rich Nuclei in Heaven and Earth
• Constraints on the high-density nuclear equation of state from the phenomenology of compact stars and heavy-ion collisions
• Dense Matter in Compact Stars: Theoretical Developments and Observational Constraints
• Nuclear matter in the crust of neutron stars
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