## PCP(BSK24)

#### Abstract

This table corresponds to the zero temperature unified equation of state (EoS) for cold non-accreting neutron stars in beta equilibrium based on the Brussels-Montreal energy- density functional BSk24 [GCP_2013]. Details on the EoS model can be found in Ref. [PCP_2018] and the routines to construct an analytical fit of the EoS are also available on the Ioffe website. The tidal deformability associated to this EoS model was calculated in Ref. [ PCS_2019]. The outer crust was calculated using the Hartree-Fock-Bogoliubov atomic mass table HFB-24 available on the BRUSLIB data base [ XGJCA_2013], except when experimental values were available, for which we used the 2016 Atomic Mass Evaluation [ WGKH_2016], supplemented by the measurements of copper isotopes from Ref. [ W_2017]. The inner crust was computed using the 4th-order Extended Thomas-Fermi (ETF) method with proton shell and pairing corrections added perturbatively via the Strutinsky integral (SI); the nucleon distributions were parametrized using damped Fermi profiles and the Coulomb energy was calculated within the Wigner-Seitz (WS) approximation. Although the EoS was originally calculated ignoring nuclear pastas, their presence in neutron-star crust was later discussed in Refs. [ PCP_2020, PC_2022] and was shown to be marginal in the Extended Thomas-Fermi plus Strutinski Integral framework [ PC_2022]. The core was assumed to be made up by an admixture of neutrons and protons neutralised by electrons and possibly by muons. ^1S_0 neutron and proton pairing gaps in neutron-star cores were calculated in Ref. [ AC_2021].

Nparam | = | 1 |

Particles | = | npemN |

T min | = | 0.0 |

T max | = | 0.0 |

T pts | = | 1 |

nb min | = | 4.68e-10 |

nb max | = | 1.49e+00 |

nb pts | = | 454 |

Y min | = | 0.0 |

Y max | = | 0.0 |

Y pts | = | 1 |

#### Nuclear Matter Properties

n_{s} |
= | 0.1578 | fm^{-3} |

E_{0} |
= | 16.048 | Mev |

K | = | 245.5 | Mev |

K' | = | 274.5 | Mev |

J | = | 30.0 | Mev |

L | = | 46.4 | Mev |

K_{sym} |
= | -37.6 | MeV |

#### Neutron Star Properties

M_{max} |
= | 2.28 | M_{sun} |

MDU,e_{} |
= | 1.595 | M_{sun} |

R_{Mmax} |
= | 11.08 | km |

R_{1.4} |
= | 12.57 | km |

#### References

##### References to the original work:

- [WGKH_2016] M. Wang, G. Audi, F. G. Kondev, W. J. Huang, S. Naimi, and X. Xu, Chinese Physics C41, 030003 (2017)
- [AC_2021] V. Allard and N. Chamel, Universe 7, 470 (2021)
- [PC_2022] J. M. Pearson and N. Chamel, Phys. Rev. C 105, 015803 (2022)
- [PCP_2020] J. M. Pearson, N. Chamel, and A. Y. Potekhin, Phys. Rev. C 101, 015802 (2020)
- [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)
- [GCP_2013] S. Goriely, N. Chamel, and J. M. Pearson, Phys. Rev. C 88, 024308 (2013)
- [PCS_2019] L. Perot, N. Chamel, and A. Sourie, Phys. Rev. C 100, 035801 (2019)
- [XGJCA_2013] Y. Xu, S. Goriely, A. Jorissen, G. L. Chen, and M. Arnould, Astronomy & Astrophysics 549, A106 (2013)
- [W_2017] A. Welker, et al, Phys. Rev. Lett. 119, 192502 (2017)

#### Data sheet

#### Data

eos.zip (0.17 MB) |

eos.zip_checksum.txt |

## Single files |

eos.t |

eos.nb |

eos.yq |

eos.compo |

eos.thermo |

eos.mr |

eos.init |

eos.micro |