We generate a second equation of state ( EOS ) of nuclear matter for a wide range of temperatures , densities , and proton fractions for use in supernovae , neutron star mergers , and black hole formation simulations .
We employ full relativistic mean field ( RMF ) calculations for matter at intermediate density and high density , and the Virial expansion of a non-ideal gas for matter at low density .
For this EOS we use the RMF effective interaction FSUGold , whereas our earlier EOS was based on the RMF effective interaction NL3 .
The FSUGold interaction has a lower pressure at high densities compared to the NL3 interaction .
We calculate the resulting EOS at over 100,000 grid points in the temperature range T = 0 to 80 MeV , the density range n _ { B } = 10 ^ { -8 } to 1.6 fm ^ { -3 } , and the proton fraction range Y _ { p } = 0 to 0.56 .
We then interpolate these data points using a suitable scheme to generate a thermodynamically consistent equation of state table on a finer grid .
We discuss differences between this EOS , our NL3 based EOS , and previous EOS by Lattimer-Swesty and H. Shen et al . for the thermodynamic properties , composition , and neutron star structure .
The original FSUGold interaction produces an EOS , that we call FSU1.7 , that has a maximum neutron star mass of 1.7 solar masses .
A modification in the high density EOS is introduced to increase the maximum neutron star mass to 2.1 solar masses and results in a slightly different EOS that we call FSU2.1 .
The EOS tables for FSU1.7 and FSU2.1 are available for download .