HS(IUF) neutron matter (no electrons)
Abstract
This is the zero electron fraction EOS table with RMF interactions IUFSU [FHPSP_2010]. Contributions of neutrons, anti-neutrons, protons, and anti-protons are included, whereas the net abundance of protons is always zero. The details of the underlying EOS model at finite electron fraction can be found in Ref. [HSNP_2010], where the TMA interactions were used. The manual from the web page at astro.physik.unibas.ch/ gives further information about the table. Applications of HS EOS for various different RMF interactions in supernova simulations can be found in Refs. [HFSLA_2012,SHF_2013].
Nparam | = | 2 |
Particles | = | np N |
T min | = | 1.00e-01 |
T max | = | 1.58e+02 |
T pts | = | 81 |
nb min | = | 1.00e-12 |
nb max | = | 1.00e+01 |
nb pts | = | 326 |
Y min | = | 0.0 |
Y max | = | 0.0 |
Y pts | = | 1 |
Nuclear Matter Properties
ns | = | 0.1546 | fm-3 |
E0 | = | 16.39 | Mev |
K | = | 231.3 | Mev |
K' | = | -290.3 | Mev |
J | = | 31.29 | Mev |
L | = | 47.2 | Mev |
Ksym | = | 28.5 | MeV |
Neutron Star Properties
Mmax | = | 1.95 | Msun |
MDU,e | = | 1.8 | Msun |
RMmax | = | 11.31 | km |
R1.4 | = | 12.7 | km |
References
References to the original work:
- [HSNP_2010] M. Hempel and J. Schaffner-Bielich, Nucl. Phys. A 837, 210 (2010)
- [FHPSP_2010] F.J. Fattoyev, C.J. Horowitz, J. Piekarewicz, and G. Shen, Phys. Rev. C 82, 055803 (2010)
Further references:
- [HFSLA_2012] M. Hempel, T. Fischer, J. Schaffner-Bielich, and M. Liebendörfer, Astrophys. J. 748, 70 (2012)
- [SHF_2013] A.W. Steiner, M. Hempel, and T. Fischer, Astrophys.J. 774,17 (2013)
Data sheet
Data
eos.zip (1.25 MB) |
eos.zip_checksum.txt |
Single files |
eos.compo |
eos.init |
eos.micro |
eos.mr |
eos.nb |
eos.t |
eos.thermo |
eos.yq |