Tables of Hyperonic Matter Equation of State for Core-Collapse Supernovae
Tables of Hyperonic Matter Equation of State for Core-Collapse Supernovae
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DOI：
10.1088/0954-3899/35/8/085201
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发表时间：
2008-02
期刊：
影响因子：
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通讯作者：
C. Ishizuka;Akira Ohnishi;Akira Ohnishi;K. Tsubakihara;K. Sumiyoshi;S. Yamada
中科院分区：
文献类型：
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作者：
C. Ishizuka;Akira Ohnishi;Akira Ohnishi;K. Tsubakihara;K. Sumiyoshi;S. Yamada
本文采用扩展的相对论平均场模型（SUf（3）RMF），在密度、温度和电荷分数等参数的广泛覆盖下，建立了一套包括超子在内的核物质状态方程，并用于对超新星坍缩过程的数值模拟。偶合常数？然后呢？超子与？介子的决定，以适应超子潜在的核物质的深度，U？(? 0)+30 MeV和U？(? 0) ? 15 MeV，这是最近对超子产生反应的分析所提出的。在低密度下，均匀物质的状态方程与Shen等人的状态方程相联系，其中有限核的形成包括在托马斯？费米近似。在目前的状态方程中，中子星的最大质量从2.17 M？(Ne?) 1.63米？(NYe?)当包含超子时。在一个球形的，绝热崩溃的15 M？星星的流体力学计算表明，由于超子的温度和密度没有达到超子混合区（T > 40 MeV或？B > 0.4 fm？3）。
We present sets of equation of state (EOS) of nuclear matter including hyperons using an SUf(3) extended relativistic mean field (RMF) model with a wide coverage of density, temperature and charge fraction for numerical simulations of core-collapse supernovae. Coupling constants of ? and ? hyperons with the ? meson are determined to fit the hyperon potential depths in nuclear matter, U?(?0) +30 MeV and U?(?0) ?15 MeV, which are suggested from recent analyses of hyperon production reactions. At low densities, the EOS of uniform matter is connected with the EOS by Shen et al, in which the formation of finite nuclei is included in the Thomas?Fermi approximation. In the present EOS, the maximum mass of neutron stars decreases from 2.17 M? (Ne?) to 1.63 M? (NYe?) when hyperons are included. In a spherical, adiabatic collapse of a 15 M? star by the hydrodynamics without neutrino transfer, hyperon effects are found to be small, since the temperature and density do not reach the region of hyperon mixture, where the hyperon fraction is above 1 % (T > 40 MeV or ?B > 0.4 fm?3).