SPG(M3) Crust NS EoS
Abstract
This inner crust EoS for β-equilibrium matter at zero temperature is con- structed with a BSk22 outer crust [ PCP_2018] below n_B = 2 × 10^−3 fm^−3 , an inner crust EoS calculated within a Compressible Liquid Drop approach [2] up to n_B = 0.79 × 10^−1 fm^−3 . The EoS parameterisation used was one of the density-dependent RMF models with the GDFM functional for the couplings [ GDFM_2008] generated in a Bayesian analysis and that agrees with both astrophysical and nuclear constraints [ SPG_2024].
| Nparam | = | 1 |
| Particles | = | npeN |
| T min | = | 0.0 |
| T max | = | 0.0 |
| T pts | = | 1 |
| nb min | = | 4.68e-10 |
| nb max | = | 7.94e-02 |
| nb pts | = | 366 |
| Y min | = | 0.0 |
| Y max | = | 0.0 |
| Y pts | = | 1 |
Nuclear Matter Properties
| ns | = | 0.161 | fm-3 |
| E0 | = | -15.8 | Mev |
| K | = | 226.0 | Mev |
| K' | = | 283.0 | Mev |
| J | = | 33.7 | Mev |
| L | = | 51.0 | Mev |
| Ksym | = | -231.0 | MeV |
Neutron Star Properties
| Mmax | = | 2.69 | Msun |
| MDU,e | = | 2.25 | Msun |
| RMmax | = | 12.42 | km |
| R1.4 | = | 12.65 | km |
References
References to the original work:
- [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)
- [GDFM_2008] P. Gögelein, E. N. E. van Dalen, C. Fuchs, and H. Müther, Phys. Rev. C 77, 025802 (2008)
- [SPG_2024] Luigi Scurto , Helena Pais, Francesca Gulminelli, arxiv:2402.15548 (2024)