Equation of State of Supernova Matter : Astrophysics and Relativity
スポンサーリンク
概要
- 論文の詳細を見る
We have calculated the equation of state of the supernova matter for various values of lepton fraction Y_L and entropy per nucleon s by using the finite temperature Thomas-Fermi model of nuclei. The pressure is dominated by degenerate pressure of leptons and the adiabatic index γ stays around 4/3. However, γ decreases by the effect of the nuclear force at the very high density region. Although the nuclei melt at rather low density, about 10^<13.9>gcm^<-3> in this calculation, the comparison with a Hartree-Fock calculation reveals that the further investigation should be done to clarify the phase transition from nuclear phase of nucleon to homogeneous phase.
- 理論物理学刊行会の論文
- 1985-02-25
著者
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OGASAWARA Ryusuke
NAOJ ALMA Chile Office, Santiago Head Office
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Ogasawara Ryusuke
Naoj Alma Chile Office Santiago Head Office
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Ogasawara R
Department Of Physics Kyoto University
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Ogasawara Ryusuke
Department Of Physics Kyoto University
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