GPPVA(NL3wrL55) NS crust
Abstract
This inner crust EoS, including nonspherical pasta phases, was calculated within a self- consistent Thomas-Fermi approach [GPPVP_2014] for beta-equilibrium matter at zero temperature. The EoS parameterisation used was the non-linear RMF NL3ωρ model with a slope of the symmetry energy, L, equal to 55 MeV [HP_2001,HPb_2001,PP_2016]. This inner crust EoS has been published in Ref.[GPPVP_2014]. For the outer crust, the EoS by Baym, Pethick and Sutherland [BPSA_1971] was added below baryon density of 0.002 fm^{−3}.
| Nparam | = | 1 |
| Particles | = | npeN |
| T min | = | 0.0 |
| T max | = | 0.0 |
| T pts | = | 1 |
| nb min | = | 6.30e-12 |
| nb max | = | 8.20e-02 |
| nb pts | = | 124 |
| Y min | = | 0.0 |
| Y max | = | 0.0 |
| Y pts | = | 1 |
Nuclear Matter Properties
| ns | = | 0.148 | fm-3 |
| E0 | = | -16.24 | Mev |
| K | = | 270.0 | Mev |
| K' | = | 198.0 | Mev |
| J | = | 31.7 | Mev |
| L | = | 55.0 | Mev |
| Ksym | = | -8.0 | MeV |
Neutron Star Properties
| Mmax | = | 2.758 | Msun |
| MDU,e | = | 0.0 | Msun |
| RMmax | = | 13.014 | km |
| R1.4 | = | 13.753 | km |
References
References to the original work:
- [GPPVP_2014] F. Grill, H. Pais, C. Providencia, I. Vidana and S. S. Avancini, Phys. Rev. C 90, 045803 (2014)
- [BPSA_1971] G. Baym, C. Pethick and P. Sutherland, Astrophys. J. 170, 299 (1971)
- [HP_2001] C. J. Horowitz and J. Piekarewicz, Phys. Rev. Lett. 86, 5647 (2001)
- [HPb_2001] C. J. Horowitz and J. Piekarewicz, Phys. Rev. C 64, 062802 (2001)
- [PP_2016] H. Pais and C. Providência, Phys. Rev. C 94, 015808 (2016)