# Rel. Mean Field and Virial EOS based on the FSU Gold interaction

The FSU gold relativistic mean filed interaction is relatively soft at high densities (low pressure).
As a result the maximum neutron star mass is of order 1.75 solar masses. We have modified the EOS above nuclear density to
have a higher pressure so that it supports a maximum neutron star mass of 2.1 solar masses (see version notes below).

### FSU version with 2.1 M_sun maximum mass:

The full EOS table including baryon, photon, and lepton contributions is in a gzip compressed ~ 100 MB file
FSU2.1eos1.01.dat.gz ,
Note that the 2.1 in the file name refers to the maximum mass.

The baryon only EOS without photon and lepton contributions is
FSU2.1eosb1.01.dat.gz

The format of these equation of state tables is described in a
FSUreadme2.1.pdf file.
A sample fortran code for reading these tables is
readeos_FSU2.1.f

###

### Original FSU version with 1.7 M_sun maximum mass:

For the unmodified EOS, the full equation of state table including baryon, photon, and lepton contributions is in a gzip compressed ~100 MB file
FSU1.7eos1.01.dat.gz

The baryon only EOS table without photon and lepton contributions is
FSU1.7eosb1.01.dat.gz

The format of these equation of state tables is described in a
FSUreadme1.7.pdf file.
A sample fortran code for reading these tables is
readeos_FSU1.7.f

###

### Version Notes: FSU based EOS

Here are short notes regarding updates to the equation of state table.

The current version of this EOS is 1.01 (as of March, 2011).

03/17/2011 Corrected error in proton chemical potential at very small proton fraction. Prepared FSU2.1eos1.01 and FSU1.7eos1.01.

11/30/2010 Changed the original FSU file name to FSU1.7eos1.0 and prepared a version FSU2.1eos1.0 that has been stiffened to yield a maximum mass of 2.1 solar masses. A term dP was added to the pressure with

dP=a(rho^2-rho_0^2)

for baryon densities rho above rho_0 =0.2 fm^-3 and dP=0 for lower densities. The constant a is a=2e-5 MeV^-2. A coresponding term was added to the energy. Note that this extra term is independent of temperature and proton fraction.

### References include:

A New Relativistic Mean Field and Virial Equation of State for Astrophysical Simulations,
G. Shen, C. J. Horowitz, and E. O`Connor, to be published, and
A New Equation of State for Astrophysical Simulations, G. Shen, C. J. Horowitz, S. Teige Phys. Rev. C **83**, 035802 (2011).
Back to Gang Shen Equations of State