### Abstract

We construct a new equation of state for baryons at sub-nuclear densities for the use in core-collapse simulations of massive stars. The formulation is based on the nuclear statistical equilibrium description and the liquid drop approximation of nuclei. The model free energy to minimize is calculated by using relativistic mean field theory for nucleons and the mass formula for nuclei with atomic number up to ∼ 1000. We have also taken into account the pasta phase. We find that the free energy and other thermodynamical quantities are not very different from those given in the standard EOSs that adopt the single nucleus approximation. On the other hand, the average mass is systematically different, which may have an important effect to the rates of electron captures and coherent neutrino scatterings on nuclei in supernova cores. It is also interesting that the root mean square of the mass number is not very different from the average mass number, since the former is important for the evaluation of coherent scattering rates on nuclei but has been unavailable so far.

Original language | English |
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Title of host publication | AIP Conference Proceedings |

Pages | 369-371 |

Number of pages | 3 |

Volume | 1484 |

DOIs | |

Publication status | Published - 2012 |

Event | International Symposium on Origin of Matter and Evolutions of Galaxies 2011, OMEG 2011 - Wako Duration: 2011 Nov 14 → 2011 Nov 17 |

### Other

Other | International Symposium on Origin of Matter and Evolutions of Galaxies 2011, OMEG 2011 |
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City | Wako |

Period | 11/11/14 → 11/11/17 |

### Fingerprint

### Keywords

- Equation of state
- Nuclear Abundances
- Nuclear Pasta
- Supernova

### ASJC Scopus subject areas

- Physics and Astronomy(all)

### Cite this

*AIP Conference Proceedings*(Vol. 1484, pp. 369-371) https://doi.org/10.1063/1.4763423

**A new baryonic equation of state at sub-nuclear densities for core-collapse simulations.** / Furusawa, Shun; Yamada, Shoichi; Sumiyoshi, Kohsuke; Suzuki, Hideyuki.

Research output: Chapter in Book/Report/Conference proceeding › Conference contribution

*AIP Conference Proceedings.*vol. 1484, pp. 369-371, International Symposium on Origin of Matter and Evolutions of Galaxies 2011, OMEG 2011, Wako, 11/11/14. https://doi.org/10.1063/1.4763423

}

TY - GEN

T1 - A new baryonic equation of state at sub-nuclear densities for core-collapse simulations

AU - Furusawa, Shun

AU - Yamada, Shoichi

AU - Sumiyoshi, Kohsuke

AU - Suzuki, Hideyuki

PY - 2012

Y1 - 2012

N2 - We construct a new equation of state for baryons at sub-nuclear densities for the use in core-collapse simulations of massive stars. The formulation is based on the nuclear statistical equilibrium description and the liquid drop approximation of nuclei. The model free energy to minimize is calculated by using relativistic mean field theory for nucleons and the mass formula for nuclei with atomic number up to ∼ 1000. We have also taken into account the pasta phase. We find that the free energy and other thermodynamical quantities are not very different from those given in the standard EOSs that adopt the single nucleus approximation. On the other hand, the average mass is systematically different, which may have an important effect to the rates of electron captures and coherent neutrino scatterings on nuclei in supernova cores. It is also interesting that the root mean square of the mass number is not very different from the average mass number, since the former is important for the evaluation of coherent scattering rates on nuclei but has been unavailable so far.

AB - We construct a new equation of state for baryons at sub-nuclear densities for the use in core-collapse simulations of massive stars. The formulation is based on the nuclear statistical equilibrium description and the liquid drop approximation of nuclei. The model free energy to minimize is calculated by using relativistic mean field theory for nucleons and the mass formula for nuclei with atomic number up to ∼ 1000. We have also taken into account the pasta phase. We find that the free energy and other thermodynamical quantities are not very different from those given in the standard EOSs that adopt the single nucleus approximation. On the other hand, the average mass is systematically different, which may have an important effect to the rates of electron captures and coherent neutrino scatterings on nuclei in supernova cores. It is also interesting that the root mean square of the mass number is not very different from the average mass number, since the former is important for the evaluation of coherent scattering rates on nuclei but has been unavailable so far.

KW - Equation of state

KW - Nuclear Abundances

KW - Nuclear Pasta

KW - Supernova

UR - http://www.scopus.com/inward/record.url?scp=84874545152&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=84874545152&partnerID=8YFLogxK

U2 - 10.1063/1.4763423

DO - 10.1063/1.4763423

M3 - Conference contribution

AN - SCOPUS:84874545152

SN - 9780735410961

VL - 1484

SP - 369

EP - 371

BT - AIP Conference Proceedings

ER -