## GPPVA(NL3wrL55) NS crust

#### Abstract

This inner crust EoS, including nonspherical pasta phases, was calculated within a self- consistent Thomas-Fermi approach [GPPVP_2014] for beta-equilibrium matter at zero temperature. The EoS parameterisation used was the non-linear RMF NL3ωρ model with a slope of the symmetry energy, L, equal to 55 MeV [HP_2001,HPb_2001,PP_2016]. This inner crust EoS has been published in Ref.[GPPVP_2014]. For the outer crust, the EoS by Baym, Pethick and Sutherland [BPSA_1971] was added below baryon density of 0.002 fm^{−3}.

Nparam | = | 1 |

Particles | = | npeN |

T min | = | 0.0 |

T max | = | 0.0 |

T pts | = | 1 |

nb min | = | 6.30e-12 |

nb max | = | 8.20e-02 |

nb pts | = | 124 |

Y min | = | 0.0 |

Y max | = | 0.0 |

Y pts | = | 1 |

#### Nuclear Matter Properties

n_{s} |
= | 0.148 | fm^{-3} |

E_{0} |
= | -16.24 | Mev |

K | = | 270.0 | Mev |

K' | = | 198.0 | Mev |

J | = | 31.7 | Mev |

L | = | 55.0 | Mev |

K_{sym} |
= | -8.0 | MeV |

#### Neutron Star Properties

M_{max} |
= | 2.758 | M_{sun} |

MDU,e_{} |
= | 0.0 | M_{sun} |

R_{Mmax} |
= | 13.014 | km |

R_{1.4} |
= | 13.753 | 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)
- [HP_2001] C. J. Horowitz and J. Piekarewicz, Phys. Rev. Lett. 86, 5647 (2001)
- [HPb_2001] C. J. Horowitz and J. Piekarewicz, Phys. Rev. C 64, 062802 (2001)
- [PP_2016] H. Pais and C. Providência, Phys. Rev. C 94, 015808 (2016)

#### Data sheet

#### Data

eos.zip (0.13 MB) |

eos.zip_checksum.txt |

## Single files |

eos.nb |

eos.t |

eos.thermo |

eos.yq |

eos.mr |