PCGS(PCSB0)
Abstract
Equation of state for cold neutron star matter in β-equilibrium containing nucleons, electrons, and muons derived using the relativistic mean field approximation. The description of the Lagrangian density and the EoS model can be found at [PCGS_2022, HTZCS_2018]. The EoS model ‘PCSB0’ results after switching off the vector self-interaction in the RMF Langrangian density given in [PCGS_2022, HTZCS_2018] (i.e, setting ζ = 0, see therein). For the crust, we have attached the crust from [HSNP_2010 ] below a baryon density(nb) < 0.069 fm−3 such that the EoS satisfies the required conditions for thermodynamic stability. The composition data is available for the core EoS only.
| Nparam | = | 1 |
| Particles | = | npeN |
| T min | = | 0.0 |
| T max | = | 0.0 |
| T pts | = | 1 |
| nb min | = | 8.93e-11 |
| nb max | = | 1.80e+00 |
| nb pts | = | 2085 |
| Y min | = | 0.0 |
| Y max | = | 0.0 |
| Y pts | = | 1 |
Nuclear Matter Properties
| ns | = | 0.15 | fm-3 |
| E0 | = | -16.0 | Mev |
| K | = | 240.0 | Mev |
| K' | = | N/A | Mev |
| J | = | 32.0 | Mev |
| L | = | 60.0 | Mev |
| Ksym | = | N/A | MeV |
Neutron Star Properties
| Mmax | = | 2.53 | Msun |
| MDU,e | = | N/A | Msun |
| RMmax | = | 12.13 | km |
| R1.4 | = | 13.3 | km |
References
References to the original work:
- [HSNP_2010] M. Hempel and J. Schaffner-Bielich, Nucl. Phys. A 837, 210 (2010)
- [HTZCS_2018] Nadine Hornick, Laura Tolos, Andreas Zacchi, Jan-Erik Christian, and Jürgen Schaffner-Bielich, Phys.Rev.C 98 (2018) 6, 065804 (2018)
- [PCGS_2022] Bikram Keshari Pradhan , Debarati Chatterjee , Radhika Gandhi , Jürgen Schaffner-Bielich, Nucl.Phys.A 1030 (2023) 122578 (2022)
Data sheet
Data
| eos.zip (0.23 MB) |
| eos.zip_checksum.txt |
Single files |
| eos.nb |
| eos.t |
| eos.yq |
| eos.thermo |
| eos.compo |
| eos.mr |
| eos.init |