## GPPVA(FSU2R) 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 FSU2R model [ NTCRD_2018]. This inner crust EoS has been published in Ref.[PFPR_2019] . For the outer crust, the BsK22 EoS by Pearson et al [PCP_2018] 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 | = | 4.68e-10 |

nb max | = | 8.29e-02 |

nb pts | = | 296 |

Y min | = | 0.0 |

Y max | = | 0.0 |

Y pts | = | 1 |

#### Nuclear Matter Properties

n_{s} |
= | 0.155 | fm^{-3} |

E_{0} |
= | 16.28 | Mev |

K | = | 238.0 | Mev |

K' | = | 135.0 | Mev |

J | = | 30.7 | Mev |

L | = | 47.0 | Mev |

K_{sym} |
= | 56.0 | MeV |

#### Neutron Star Properties

M_{max} |
= | 2.048 | M_{sun} |

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

R_{Mmax} |
= | 11.73 | km |

R_{1.4} |
= | 12.98 | 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)
- [NTCRD_2018] R. Negreiros, L. Tolos, M. Centelles, A. Ramos, and V. Dexheimer, Astrophys. J. 863, 104 (2018)
- [PFPR_2019] C. Providência, M. Fortin, H. Pais, and A. Rabhi, Astron. Space Sci. 6, 13 (2019)
- [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)

#### Data sheet

#### Data

eos.zip (0.14 MB) |

eos.zip_checksum.txt |

## Single files |

eos.init |

eos.nb |

eos.t |

eos.yq |

eos.thermo |

eos.compo |

eos.mr |