VGBCMR(D1MStar)
Abstract
This EoS table corresponds to the data and model in [ MVCD_2020, VGCMR_2021]. The Gogny D1M∗ effective interaction [ GCVR_2018] is used. The EoS in the inner crust is obtained with the Wigner-Seitz approximation in the Variational Wigner-Kirkwood approach along with the Strutinsky integral method, which allows one to estimate in a perturbative way the proton shell and pairing corrections. For the outer crust, the EoS is determined basically by the nuclear masses, which are taken from the experiments, wherever they are available, or by HFB calculations performed with this new force if the experimental masses are not known. The leptonic sector accounts for electrons and muons.
| Nparam | = | 1 |
| Particles | = | npemN |
| T min | = | 0.0 |
| T max | = | 0.0 |
| T pts | = | 1 |
| nb min | = | 6.78e-13 |
| nb max | = | 1.40e+00 |
| nb pts | = | 2221 |
| Y min | = | 0.0 |
| Y max | = | 0.0 |
| Y pts | = | 1 |
Nuclear Matter Properties
| ns | = | 0.165 | fm-3 |
| E0 | = | 16.06 | Mev |
| K | = | 225.4 | Mev |
| K' | = | N/A | Mev |
| J | = | 30.25 | Mev |
| L | = | 43.18 | Mev |
| Ksym | = | N/A | MeV |
Neutron Star Properties
| Mmax | = | 2.0 | Msun |
| MDU,e | = | 1.96 | Msun |
| RMmax | = | 10.2 | km |
| R1.4 | = | 11.71 | km |
References
References to the original work:
- [VGCMR_2021] X. Vinas, C. Gonzalez-Boquera, M. Centelles, C. Mondal and L. M. Robledo, Symmetry 13, 1613 (2021)
- [MVCD_2020] C. Mondal, X. Vinas, M. Centelles and J. N. De, Phys. Rev. C 102,015802 (2020)
- [GCVR_2018] C. Gonzalez-Boquera, M. Centelles, X. Vinas, L. M. Robledo, Phys. Lett. B 779, 195. (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 |