### Abstract

We construct the equations of state for baryons at sub-nuclear densities for the use in core-collapse simulations of massive stars. The abundance of various nuclei is obtained together with the ther-modynamic quantities. The formulation is the NSE description and the liquid drop approximation of nuclei. The model free energy to minimize is calculated by relativistic mean field theory for nucleons and the mass formula for nuclei with the atomic number up to ∼ 1000. We have also taken into account the pasta phase for heavy nuclei and the contribution of Pauli energies between free nucleons to binding energies to light nuclei. The experimental and theoretical mass data are employed to evaluate the shell effects of nuclei. We find that the abundance of heavy nuclei is different depending on shell effects of nuclei, which may have an important effect to the rates of electron captures and coherent neutrino scatterings on nuclei in supernova cores. The Pauli and self energy shifts also affect the abundance of light nuclei by comparing with ordinary nuclear statistical equilibrium results, which may affect the heating and cooling rates of supernova cores and shocked envelopes.

Original language | English |
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Title of host publication | Proceedings of Science |

Publication status | Published - 2012 |

Event | 12th International Symposium on Nuclei in the Cosmos, NIC 2012 - Cairns, QLD, Australia Duration: 2012 Aug 5 → 2012 Aug 12 |

### Other

Other | 12th International Symposium on Nuclei in the Cosmos, NIC 2012 |
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Country | Australia |

City | Cairns, QLD |

Period | 12/8/5 → 12/8/12 |

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### ASJC Scopus subject areas

- General

### Cite this

*Proceedings of Science*

**A new equation of state with abundances of all nuclei in core collapse simulations of massive stars.** / Furusawa, Shun; Sumiyoshi, Kohsuke; Yamada, Shoichi; Suzuki, Hideyuki.

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

*Proceedings of Science.*12th International Symposium on Nuclei in the Cosmos, NIC 2012, Cairns, QLD, Australia, 12/8/5.

}

TY - GEN

T1 - A new equation of state with abundances of all nuclei in core collapse simulations of massive stars

AU - Furusawa, Shun

AU - Sumiyoshi, Kohsuke

AU - Yamada, Shoichi

AU - Suzuki, Hideyuki

PY - 2012

Y1 - 2012

N2 - We construct the equations of state for baryons at sub-nuclear densities for the use in core-collapse simulations of massive stars. The abundance of various nuclei is obtained together with the ther-modynamic quantities. The formulation is the NSE description and the liquid drop approximation of nuclei. The model free energy to minimize is calculated by relativistic mean field theory for nucleons and the mass formula for nuclei with the atomic number up to ∼ 1000. We have also taken into account the pasta phase for heavy nuclei and the contribution of Pauli energies between free nucleons to binding energies to light nuclei. The experimental and theoretical mass data are employed to evaluate the shell effects of nuclei. We find that the abundance of heavy nuclei is different depending on shell effects of nuclei, which may have an important effect to the rates of electron captures and coherent neutrino scatterings on nuclei in supernova cores. The Pauli and self energy shifts also affect the abundance of light nuclei by comparing with ordinary nuclear statistical equilibrium results, which may affect the heating and cooling rates of supernova cores and shocked envelopes.

AB - We construct the equations of state for baryons at sub-nuclear densities for the use in core-collapse simulations of massive stars. The abundance of various nuclei is obtained together with the ther-modynamic quantities. The formulation is the NSE description and the liquid drop approximation of nuclei. The model free energy to minimize is calculated by relativistic mean field theory for nucleons and the mass formula for nuclei with the atomic number up to ∼ 1000. We have also taken into account the pasta phase for heavy nuclei and the contribution of Pauli energies between free nucleons to binding energies to light nuclei. The experimental and theoretical mass data are employed to evaluate the shell effects of nuclei. We find that the abundance of heavy nuclei is different depending on shell effects of nuclei, which may have an important effect to the rates of electron captures and coherent neutrino scatterings on nuclei in supernova cores. The Pauli and self energy shifts also affect the abundance of light nuclei by comparing with ordinary nuclear statistical equilibrium results, which may affect the heating and cooling rates of supernova cores and shocked envelopes.

UR - http://www.scopus.com/inward/record.url?scp=84887416285&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=84887416285&partnerID=8YFLogxK

M3 - Conference contribution

AN - SCOPUS:84887416285

BT - Proceedings of Science

ER -