## GPPVA(TM1e) 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 TM1e model [SJHS_2020]. This inner crust EoS has been used in Ref. [BPAP_2021]. 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 | = | 8.90e-02 |

nb pts | = | 131 |

Y min | = | 0.0 |

Y max | = | 0.0 |

Y pts | = | 1 |

#### Nuclear Matter Properties

n_{s} |
= | 0.145 | fm^{-3} |

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

K | = | 281.0 | Mev |

K' | = | -285.0 | Mev |

J | = | 31.4 | Mev |

L | = | 40.0 | Mev |

K_{sym} |
= | 3.57 | MeV |

#### Neutron Star Properties

M_{max} |
= | 2.12 | M_{sun} |

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

R_{Mmax} |
= | 11.88 | km |

R_{1.4} |
= | 13.16 | 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)
- [SJHS_2020] H. Shen, F. Ji, J. Hu, K. Sumiyoshi, arXiv:2001.10143 (2020)
- [BPAP_2021] O. Boukari, H. Pais, S. Antić, and C. Providência, Phys. Rev. C 103, 055804 (2021)

#### Data sheet

#### Data

eos.zip (0.12 MB) |

eos.zip_checksum.txt |

## Single files |

eos.init |

eos.nb |

eos.t |

eos.yq |

eos.thermo |

eos.mr |