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 J0348+0432 measured by Antoniadis et al., Science 340 (2013). 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. Please contact 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 (29.01.2015).
The EOS tables and corresponding drivers are also availabe on www.stellarcollapse.org, in a format for use in the
GR1D 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.
The EOS tables are given in two different formats:
Furthermore, there are routines for the full nuclear composition:
and tables with single-particle properties of unbound nucleons, which are required, e.g., for weak charge current rates:
|RMF interactions/mass table||extended format||nuclear composition||Shen 98 format||single-particle properties|
|TMA/Geng et al.||tma_geng_bin.zip||tma_geng_comp.zip||tma_geng_shen98format.zip||tma_geng_spp.zip|
|TM1/Geng et al.||tm1_geng_bin.zip||tm1_geng_comp.zip||tm1_geng_shen98format.zip||tm1_geng_spp.zip|
|NL3/Lalazissis et al.||nl3_lala_bin.zip||nl3_lala_comp.zip||nl3_lala_shen98format.zip||nl3_lala_spp.zip|
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. The passwords for these tables are "sneos_a", "sneos_ad", and "sneos_adt":
|considered light nuclei||extended format||nuclear composition||Shen 98 format|
|only alphas and deuterons||tm1_geng_bin_ad.zip||tm1_geng_comp_ad.zip||tm1_geng_shen98format_ad.zip|
|only alphas, deuterons and tritons||tm1_geng_bin_adt.zip||tm1_geng_comp_adt.zip||tm1_geng_shen98format_adt.zip|
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 section.
Department of Physics
University of Basel