## BL(chiral) with crust

#### Abstract

Microscopic equation of state (EoS) of dense beta-stable nuclear matter at zero temperature (T=0) obtained using realistic two-body and three-body nuclear interactions derived in the framework of chiral perturbation theory (ChPT) and including the Delta(1232) isobar intermediate state. This EoS has been derived using the Brueckner-Bethe-Goldstone quantum many-body theory in the Brueckner-Hartree-Fock approximation with the continuous choice for the auxiliary single particle potential. The present table is relative to the nuclear interaction model denoted as N3LODelta+N2LODelta in [BL_2018]. It contains the contributions from electrons and muons in addition to beta-stable nuclear matter. Below a density of n_B = 0.08 fm^(-3), the crust EoS from Douchin and Haensel [DHA_2001] has been added.

Nparam | = | 1 |

Particles | = | npem |

T min | = | 0.0 |

T max | = | 0.0 |

T pts | = | 1 |

nb min | = | 7.93e-15 |

nb max | = | 1.29e+00 |

nb pts | = | 283 |

Y min | = | 0.0 |

Y max | = | 0.0 |

Y pts | = | 1 |

#### Nuclear Matter Properties

n_{s} |
= | 0.171 | fm^{-3} |

E_{0} |
= | 15.23 | Mev |

K | = | 190.0 | Mev |

K' | = | 0.0 | Mev |

J | = | 35.39 | Mev |

L | = | 76.0 | Mev |

K_{sym} |
= | 0.0 | MeV |

#### Neutron Star Properties

M_{max} |
= | 2.08 | M_{sun} |

MDU,e_{} |
= | 0.961 | M_{sun} |

R_{Mmax} |
= | 10.26 | km |

R_{1.4} |
= | 12.31 | km |

#### References

#### Data sheet

#### Data

eos.zip (0.14 MB) |

eos.zip_checksum.txt |

## Single files |

eos.compo |

eos.init |

eos.mr |

eos.nb |

eos.t |

eos.thermo |

eos.yq |