Equations of State
This figure shows the mass-radius relation for cold neutron stars in beta-equilibrium for the supernova EOS tables from below, two EOS by Lattimer and Swesty, NPA 535 (1991) (LS180 and LS220), and Shen et al., PTP 100 (1998) (STOS). The horizontal lines show the constraint from pulsar PSR J1614-2230 measured by Demorest et al., Nature 467 (2010). The grey shaded regions show the one- and two-sigma regions from neutron star observations derived by Steiner et al., ApJ 722 (2010).
All tables are compressed zip-files. Some of the older files still have a password protection, which I will remove soon. For the DD2 tables, the password is "sneos_dd2", for the other tables it is "sneos" or there is none.
me if you have any questions. If you have problems with opening the binary files, I can also provide you ASCII tables. The EOS tables are calculated including all heavy and light nuclei which are available in the corresponding mass tables, if not stated otherwise. For more details see the Manual v1.04
and the list of References
. You might also want to have a look at the Version history (16.01.2014)
The EOS tables and corresponding drivers are also availabe on www.stellarcollapse.org
, in a format for use in the
code provided by the Caltech computational relativistic astrophysics group. Below you find the original tables which were used as input on www.stellarcollapse.org
The EOSs are also listed in the CompOSE database, http://compose.obspm.fr
, in a special advanced format. CompOSE is the EOS database from the Compstar network and it provides a comprehensive and very useful EOS manual and also table interpolation.
Recent versions (v1.0 - v1.04):
The EOS tables are given in two different formats:
- extended format: EOS tables in extended format with electrons and photons as zipped binary files (created with ifort on a 64bit machine)
- Shen 98 format: EOS tables in Shen 98 format without electrons and photons as zipped ASCII files
Furthermore, there are routines for the full nuclear composition:
- nuclear composition: Zipped Fortran composition modules and binary data files (created
with ifort on a 64bit machine)
Special treatment of light nuclei
In the following you find links to EOS tables for TM1/Geng et al., in which only a selection of light nuclei with Z ≤ 5 is included:
Nuclear composition for the simulation of the core-collapse supernova of the 15 Msun
progenitor from Woosley and Weaver (1995) and the TM1 EOS. Simulation performed by T. Fischer (GSI, Darmstadt). Description of the used core collapse model (spherically symmetric, general relativistic radiation hydrodynamics and three flavor Boltzmann neutrino transport in Fischer et al. (2009) and references therein. The shown time is the post-bounce time. Note that the animation time scale is set by the time-steps used in the simulation. For details, see the article New equations of state in core-collapse supernova simulations
in the reference
Outer crust of cold neutron stars — ISOLTRAP+AME2012
- Kreim, S.; Hempel, M.; Lunney, D.; Schaffner-Bielich, J.
Nuclear Masses and Neutron Stars
Accepted for publication in Int. J. Mass. Spectrom. (2013)
Outer crust of cold neutron stars — AME2003
- Rüster, S. B.; Hempel, M.; Schaffner-Bielich, J.
Outer crust of nonaccreting cold neutron stars
Phys. Rev. C 73, 035804 (2006)
NASA ADS URL
- Guo, L.; Hempel, M.; Schaffner-Bielich, J.; Maruhn, J. A.
Triaxial nuclear models and the outer crust of nonaccreting cold neutron stars
Phys. Rev. C 76, 065801 (2007)
NASA ADS URL