Revisiting the hot matter in the center of gamma-ray bursts and supernovae
Revisiting the hot matter in the center of gamma-ray bursts and supernovae
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DOI：
10.1051/0004-6361/201321705
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发表时间：
2013-05
影响因子：
6.5
通讯作者：
Ang Li;Tong Liu
中科院分区：
文献类型：
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作者：
Ang Li;Tong Liu
目标。在伽马射线暴中，或在成功超新星的原中子星诞生过程中，中微子占主导地位的吸积流的内部区域可以产生带有核子的热物质。物质的组成和状态方程取决于不同中微子不透明度下的动态β平衡。核子之间的强相互作用也可能起到重要作用。我们计划通过将这两个方面纳入我们的模型来扩展之前的研究。方法：研究方法。用一个介于中微子自由逃逸情况和中微子囚禁情况之间的平衡因子X来模拟中微子光学薄到厚的β平衡条件。我们使用扩展到有限温度区域的微观Brueckner-Hartree-Fock方法来研究相互作用的核子。结果。在β平衡的各个阶段，我们给出了不同密度和温度下热核物质的组成和化学势。我们还将我们的实际状态方程与自由气体模型的状态方程进行比较。我们发现，适当地描述中微子的不透明度和核子之间的强相互作用是很重要的，在模型计算中应该考虑它们。
Aims. Hot matter with nucleons can be produced in the inner region of the neutrino-dominated accretion flow in gamma-ray bursts or during the proto-neutron star birth in successful supernovae. The composition and equation of state of the matter depend on the dynamic beta equilibrium under various neutrino opacities. The strong interaction between nucleons may also play an important role. We plan to extend the previous studies by incorporating these two aspects in our model. Methods. The modification of the beta-equilibrium condition from neutrino optically thin to thick was modeled by an equilibrium factor chi ranging between the neutrino-freely-escaping case and the neutrino-trapped case. We employed the microscopic Brueckner-Hartree-Fock approach extended to the finite temperature regime to study the interacting nucleons. Results. We show the composition and chemical potentials of the hot nuclear matter for different densities and temperatures at each stage of beta equilibrium. We also compare our realistic equation of states with those of the free-gas model. We find that it is important to properly describe the neutrino opacity and the strong interaction between nucleons, and they should be taken into account in model calculations.