## PCGS(PCSB1)

#### Abstract

Equation of state for cold neutron star matter in β-equilibrium containing nucleons, electrons, and muons derived using the relativistic mean field approximation. The description of the Lagrangian density and the EoS model can be found at [PCGS_2022, HTZCS_2018]. The EoS model ‘PCSB1’ results after setting ζ = 0.01 in the RMF Langrangian density given in [PCGS_2022] (i.e., keeping the vector self-interaction strength non-zero and finite, see therein). For the crust, we have attached the crust from [HSNP_2010 ] below a baryon density(nb) < 0.069 fm−3 such that the EoS satisfies the required conditions for thermodynamic stability. The composition data is available for the core EoS only.

Nparam | = | 1 |

Particles | = | npemN |

T min | = | 0.0 |

T max | = | 0.0 |

T pts | = | 1 |

nb min | = | 8.93e-11 |

nb max | = | 1.80e+00 |

nb pts | = | 1795 |

Y min | = | 0.0 |

Y max | = | 0.0 |

Y pts | = | 1 |

#### Nuclear Matter Properties

n_{s} |
= | 0.15 | fm^{-3} |

E_{0} |
= | -16.0 | Mev |

K | = | 240.0 | Mev |

K' | = | N/A | Mev |

J | = | 32.0 | Mev |

L | = | 60.0 | Mev |

K_{sym} |
= | N/A | MeV |

#### Neutron Star Properties

M_{max} |
= | 2.19 | M_{sun} |

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

R_{Mmax} |
= | 11.73 | km |

R_{1.4} |
= | 13.25 | km |

#### References

##### References to the original work:

- [HSNP_2010] M. Hempel and J. Schaffner-Bielich, Nucl. Phys. A 837, 210 (2010)
- [HTZCS_2018] Nadine Hornick, Laura Tolos, Andreas Zacchi, Jan-Erik Christian, and Jürgen Schaffner-Bielich, Phys.Rev.C 98 (2018) 6, 065804 (2018)
- [PCGS_2022] Bikram Keshari Pradhan , Debarati Chatterjee , Radhika Gandhi , Jürgen Schaffner-Bielich, Nucl.Phys.A 1030 (2023) 122578 (2022)

#### Data sheet

#### Data

eos.zip (0.22 MB) |

eos.zip_checksum.txt |

## Single files |

eos.nb |

eos.t |

eos.yq |

eos.compo |

eos.thermo |

eos.init |

eos.mr |