HS(TMA) neutron matter (no electrons)
Abstract
This is the zero electron fraction EOS table with RMF interactions TMA [THSSN_1995]. 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]. 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 | = | 0.1472 | fm-3 |
| E0 | = | 16.03 | Mev |
| K | = | 318.2 | Mev |
| K' | = | -572.2 | Mev |
| J | = | 30.66 | Mev |
| L | = | 90.14 | Mev |
| Ksym | = | 10.7 | MeV |
Neutron Star Properties
| Mmax | = | 2.02 | Msun |
| MDU,e | = | 1.2 | Msun |
| RMmax | = | 12.1 | km |
| R1.4 | = | 13.8 | km |
References
References to the original work:
- [THSSN_1995] H. Toki, D. Hirata, Y. Sugahara, K. Sumiyoshi, and I. Tanihata, Nucl. Phys. A 588, 357 (1995)
- [HSNP_2010] M. Hempel and J. Schaffner-Bielich, Nucl. Phys. A 837, 210 (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)