## ABHT(QMC-RMF2)

#### Abstract

An EoS in β-equilibrium at T = 0. The core is homogeneous n, p, e matter that begins above 0.07 fm^−3. It is computed using a relativistic mean-field theory constrained by chiral effective field theory calculations of pure neutron matter (from 0.08 fm^−3 to 0.32 fm^−3) and by properties of isospin-symmetric nuclear matter around saturation density [ABHT_2022 ]. The outer crust is the Baym-Pethick-Sutherland (BPS) EoS and spans the density range 6.30 × 10^−12 fm^−3 to 2.57 × 10^−4 fm^−3 [BPSA_1971]. The inner crust is the GPPVA(TM1e) EoS, which models nuclear pasta phases calculated within a self-consistent Thomas- Fermi approach from 2.00 × 10^−3 fm^−3 to 6.24 × 10^−2 fm^−3 [GPPVP_2014]. A first-order phase transition to the core is imposed at a baryon chemical potential of 952.22 MeV.

Nparam | = | 1 |

Particles | = | npeN |

T min | = | 0.0 |

T max | = | 0.0 |

T pts | = | 1 |

nb min | = | 6.30e-11 |

nb max | = | 1.28e+00 |

nb pts | = | 301 |

Y min | = | 0.0 |

Y max | = | 0.0 |

Y pts | = | 1 |

#### Nuclear Matter Properties

n_{s} |
= | 0.161 | fm^{-3} |

E_{0} |
= | -16.3 | Mev |

K | = | 264.0 | Mev |

K' | = | 450.0 | Mev |

J | = | 32.7 | Mev |

L | = | 40.6 | Mev |

K_{sym} |
= | -170.0 | MeV |

#### Neutron Star Properties

M_{max} |
= | 2.04 | M_{sun} |

MDU,e_{} |
= | N/A | M_{sun} |

R_{Mmax} |
= | 10.49 | km |

R_{1.4} |
= | 12.03 | 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)
- [ABHT_2022] M. G. Alford, L. Brodie, A. Haber, and I. Tews, Phys. Rev. C 106, 055804 (2022)

#### Data sheet

#### Data

eos.zip (0.15 MB) |

eos.zip_checksum.txt |

## Single files |

eos.mr |

eos.compo |

eos.init |

eos.micro |

eos.thermo |

eos.t |

eos.nb |

eos.yq |