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A new equation of state Based on Nuclear Statistical Equilibrium for Core-Collapse Simulations

Published online by Cambridge University Press:  05 September 2012

Shun Furusawa ,
Shoichi Yamada ,
Kohsuke Sumiyoshi  and
Hideyuki Suzuki
Shun Furusawa
Affiliation:
Department of Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan email: furusawa@heap.phys.waseda.ac.jp
Shoichi Yamada
Affiliation:
Department of Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan email: furusawa@heap.phys.waseda.ac.jp Advanced Research Institute for Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan
Kohsuke Sumiyoshi
Affiliation:
Numazu College of Technology, Ooka 3600, Numazu, Shizuoka 410-8501, Japan
Hideyuki Suzuki
Affiliation:
Faculty of Science and Technology, Tokyo University of Science, Yamazaki 2641, Noda, Chiba 278-8510, Japan
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Abstract

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We calculate a new equation of state for baryons at sub-nuclear densities for the use in core-collapse simulations of massive stars. The formulation is the nuclear statistical equilibrium 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 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 on the rates of electron captures and coherent neutrino scatterings on nuclei in supernova cores.

Keywords

equation of statedense matternuclear abundances & supernovae
Type
Poster Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Symposium S279: Death of Massive Stars: Supernovae and Gamma-Ray Bursts , April 2011 , pp. 333 - 334
Copyright
Copyright © International Astronomical Union 2012

References

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