A Complete Equation of State for Astrophysical Simulations

Abstract

We construct a complete equation of state (EOS) covering a wide range of temperature, proton fraction, and baryon density for the use of astrophysical simulations. We employ the relativistic mean-field (RMF) theory to describe nuclear interactions and adopt the Thomas-Fermi approximation to describe the nonuniform nuclear matter. The uniform matter and nonuniform matter are studied consistently using the same RMF theory.

Comments: 3 pages, 1 figure, Proceedings of "Quarks and Compact Stars" (QCS 2014)