Microphysics: Equation of State
The EOS routines and tables were put together by Christian D. Ott and Evan O'Connor. Please feel free to use them, but please make reference to Evan O’Connor and Christian D. Ott, A New Spherically-Symmetric General Relativistic Hydrodynamics Code for Stellar Collapse to Neutron Stars and Black Holes, Class. Quant. Grav., 27 114103, 2010, and, of course, the original authors of the EOS.
If you have any questions or have discovered a bug in our routines/tables, please e-mail us at .
Disclaimer: Please note that the routines and tables provided here come with absolutely no warranty and we are unable to guarantee that we will be able to provide support or help if you run into problems integrating them with your simulation code. If you decide to use the provided EOS routines and data in published work, it is YOUR responsibility to check their physical correctness and consistency.
Licensing: For the time being (until licensing issue are sorted out), we release the code under the creative commons attribution-noncommercial-share alike
This means that you may use the code and tables, but must make reference to our work, must not use them for commercial purposes, and any code including or using our routines or part of them may be made publicly available, and if so, only under the same license.
- Equation of state maker routines:
Fortran 90 routines that allow you to read in original EOS tables (i.e. H. Shen et al. 2011 or G. Shen et al. 2011ab) and construct an .h5 table compatible with EOSdriver. This is available via anonymous svn checkout:
svn checkout --username anon --password anon svn://stellarcollapse.org/projects/EOSmaker
- Equation of state driver routines:
Fortran 90 routines that allow you to read in our EOS tables and that contain various routines for interpolation and EOS inversion are available via anonymous svn checkout:
svn checkout --username anon --password anon svn://stellarcollapse.org/projects/EOSdriver
- Equation of State Tables:
We provide tables for the nuclear equations of state of Lattimer and Swesty (1991), H. Shen et al. (2011), G. Shen et al. (2011ab), and Hempel et al. (2012), Steiner et al. (2012). Details on the tables and how they were generated (with EOSmaker above) can be found in Evan O’Connor and Christian D. Ott, Class. Quant. Grav., 27 114103, 2010. The tables are provided in bzip2-compressed HDF5 format and are 200-350 MB in size and can be accessed most easily with EOSdriver.
EOS variant Table name and link Lattimer and Swesty EOS, website LS EOS, K = 180 MeV LS180_234r_136t_50y_analmu_20091212_SVNr26.h5.bz2 LS EOS, K = 220 MeV LS220_234r_136t_50y_analmu_20091212_SVNr26.h5.bz2 LS EOS, K = 375 MeV LS375_234r_136t_50y_analmu_20091212_SVNr26.h5.bz2 LS EOS, K = 220 MeV, higher resolution, lower range& LS220_240r_140t_50y_analmu_20120628_SVNr28.h5.bz2 H. Shen et al. EOS, website H. Shen EOS (2011, EOS2) HShenEOS_rho220_temp180_ye65_version_1.1_20120817.h5.bz2 H. Shen EOS with Hyperons (2011, EOS3) HShen_HyperonEOS_rho220_temp180_ye65_version_1.1_20131007.h5.bz2 G. Shen et al. EOS (NL3) G. Shen et al. EOS (FSU), website GShen EOS, NL3 GShen_NL3EOS_rho280_temp180_ye52_version_1.1_20120817.h5.bz2 GShen EOS, FSU1.7 GShenFSU_1.7EOS_rho280_temp180_ye52_version_1.1_20120817.h5.bz2 GShen EOS, FSU2.1 GShenFSU_2.1EOS_rho280_temp180_ye52_version_1.1_20120824.h5.bz2 Hempel et al. EOS**, website HS EOS, TMA Hempel_TMAEOS_rho234_temp180_ye60_version_1.1_20120817.h5.bz2 HS EOS, TM1 Hempel_TM1EOS_rho234_temp180_ye60_version_1.1_20120817.h5.bz2 HS EOS, FSG Hempel_FSGEOS_rho234_temp180_ye60_version_1.1_20120817.h5.bz2 HS EOS, NL3 Hempel_NL3EOS_rho234_temp180_ye60_version_1.1_20120817.h5.bz2 HS EOS, DD2 Hempel_DD2EOS_rho234_temp180_ye60_version_1.1_20120817.h5.bz2 HS EOS, IUF Hempel_IUFEOS_rho234_temp180_ye60_version_1.1_20140129.h5.bz2 Steiner et al. EOS**, website SFH EOS, SFHo Hempel_SFHoEOS_rho222_temp180_ye60_version_1.1_20120817.h5.bz2 SFH EOS, SFHx Hempel_SFHxEOS_rho234_temp180_ye60_version_1.1_20120817.h5.bz2 &This table sacrifices range for resolution. It extends to log(density) = 15 instead of 16, and 50MeV instead of 250MeV in temperature. It also has slightly more points. This EOS was used for the FLASH simulations in Couch & Ott (2013) and Couch & O'Connor (2014) **Please be aware that the Hempel et al. and Steiner et al. EOS have light nuclei in addition to neutron, protons, alphas and a characteristic heavy nucleus. These include deutrons, tritons, helions, and 4Li nuclei. They affect the compositions, and therefore neutrino interactions. All eight mass fractions are available in the H5 table, however the EOSdriver routines must be modified to access them. *August 14th, 2012 (and then 17th) update fixed small issues in the electron chemical potential (and electron EOS) at the low density interface (everywhere) *August 24th, 2012: The FSU2.1 was actually the FSU1.7, fixed now. *October 7th, 2013: Added the H. Shen EOS with Hyperons. Note, the hyperon mass fraction can be found via 1-xn-xp-xa-xh.