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arXiv 0706.0698nucl-th
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动量相关有效相互作用下核对称能的热效应

Thermal effects on nuclear symmetry energy with a momentum-dependent effective interaction

Ch. C. Moustakidis

摘要:

热丰中子物质的核对称能对于理解大质量恒星的动力学演化和超新星爆炸机制具有重要意义。特别是,在超新星爆发前的原子核和/或自由质子上的电子俘获率对有限温度下的对称能特别敏感。鉴于上述,在本工作中,我们计算的对称性能量作为温度的函数的重子密度的各种值,通过应用动量相关的有效相互作用。除了以前的工作,热效应分别研究在动力学部分和相互作用部分的对称能。我们还专注于平均场势的计算,广泛应用于重离子反应的研究,无论是核和纯中子物质。质子分数和电子化学势,这是代表超新星和中子星的热演化的关键量,计算了不同的温度值。最后,我们构造了一个与温度有关的$β$ -稳定核物质状态方程,它是评价中子星性质的基本成分。

英文摘要:

The knowledge of the nuclear symmetry energy of hot neutron-rich matter is important for understanding the dynamical evolution of massive stars and the supernova explosion mechanisms. In particular, the electron capture rate on nuclei and/or free protons in presupernova explosions is especially sensitive to the symmetry energy at finite temperature. In view of the above, in the present work we calculate the symmetry energy as a function of the temperature for various values of the baryon density, by applying a momentum-dependent effective interaction. In addition to a previous work, the thermal effects are studied separately both in the kinetic part and the interaction part of the symmetry energy. We focus also on the calculations of the mean field potential, employed extensively in heavy ion reaction research, both for nuclear and pure neutron matter. The proton fraction and the electron chemical potential, which are crucial quantities for representing the thermal evolution of supernova and neutron stars, are calculated for various values of the temperature. Finally, we construct a temperature dependent equation of state of $β$-stable nuclear matter, the basic ingredient for the evaluation of the neutron star properties.

机构、总结、中文摘要均由AI分析而来,可能存在错误,请以论文正文为准。

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