Second relativistic mean field and virial equation of state for astrophysical simulations
- Creators
- Shen, G.
- Horowitz, C. J.
- O'Connor, E.
Abstract
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 nonideal 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 EOSs by Lattimer-Swesty and H. Shen et al. for the thermodynamic properties, composition, and neutron star structure. The original FSUGold interaction produces an EOS, which 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.
Additional Information
© 2011 American Physical Society. Received 26 March 2011; revised 16 May 2011; published 23 June 2011. We thank Lorenz Hüdepohl, Thomas Janka, Andreas Marek, and Christian Ott for important help running astrophysical simulations to debug our EOS and Scott Teige for help on shell script for running the job on the Teragrid supercomputer cluster Ranger. This work was supported in part by DOE Grant No. DE-FG02-87ER40365 and Teragrid Grant No.PHY100015 for computing time. The work of G.S. was also supported in part by a grant from the DOE under Contract No.DE-AC52-06NA25396 and the DOE topical collaboration to study "Neutrinos and nucleosynthesis in hot and densematter."Attached Files
Published - Shen2011p14626Phys_Rev_C.pdf
Supplemental Material - FSU1.7eos1.01.dat.gz
Supplemental Material - FSU1.7eosb1.01.dat.gz
Supplemental Material - FSU2.1eos1.01.dat.gz
Supplemental Material - FSU2.1eosb1.01.dat.gz
Supplemental Material - FSUreadme1.7.pdf
Supplemental Material - FSUreadme2.1.pdf
Supplemental Material - README.TXT
Supplemental Material - readeos_FSU1.7.f
Supplemental Material - readeos_FSU2.1.f
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Additional details
- Eprint ID
- 24406
- Resolver ID
- CaltechAUTHORS:20110713-105144350
- DE-FG02-87ER40365
- Department of Energy (DOE)
- PHY100015
- Teragrid
- DE-AC52-06NA25396
- Department of Energy (DOE)
- Created
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2011-07-13Created from EPrint's datestamp field
- Updated
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2021-11-09Created from EPrint's last_modified field