GPPVA(FSU2) 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 FSU2 model [CP_2014]. This inner crust EoS has been published in Ref. [PFPR_2019]. For the outer crust, the BsK22 EoS by Pearson et al [PCP_2018] 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 | = | 4.68e-10 |
| nb max | = | 5.40e-02 |
| nb pts | = | 269 |
| Y min | = | 0.0 |
| Y max | = | 0.0 |
| Y pts | = | 1 |
Nuclear Matter Properties
| ns | = | 0.1505 | fm-3 |
| E0 | = | -16.28 | Mev |
| K | = | 238.0 | Mev |
| K' | = | -149.0 | Mev |
| J | = | 37.6 | Mev |
| L | = | 113.0 | Mev |
| Ksym | = | 25.0 | MeV |
Neutron Star Properties
| Mmax | = | 2.07 | Msun |
| MDU,e | = | N/A | Msun |
| RMmax | = | 12.08 | km |
| R1.4 | = | 13.89 | 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)
- [PFPR_2019] C. Providência, M. Fortin, H. Pais, and A. Rabhi, Astron. Space Sci. 6, 13 (2019)
- [CP_2014] W.-C. Chen and J. Piekarewicz, Phys. Rev. C 90, 044305 (2014)
- [PCP_2018] J. M. Pearson, N. Chamel, A. Y. Potekhin, A. F. Fantina, C. Ducoin, A. K. Dutta, and S. Goriely, MNRAS 481, 2994 (2018)
Data sheet
Data
| eos.zip (0.14 MB) |
| eos.zip_checksum.txt |
Single files |
| eos.init |
| eos.nb |
| eos.t |
| eos.yq |
| eos.thermo |
| eos.compo |
| eos.mr |