Thermal Dynamics Behavior of Protoneutron Star Matter

In the relativistic σ-ω model, including the vacuum fluctuation of nucleons and σ mesons, the effect of the temperature to the composition and equation of state of protoneutron star matter, nucleon effective mass and chemical potential of neutrons and electrons are studied. We find that the influence of the temperature on the equation of state of protoneutron star matter is indeed small, however, its influence on the composition of protoneutron star, which will contribute to the evolution of protoneutron star, cannot be neglected in low density region. The chemical potentials of neutrons and electrons also depend on the temperature in almost the same density region.

质子中子星物质的热力学性质(英文)

在相对论σ-ω-ρ模型的平均场近似下,研究了质子中子星物质在均熵状态下的组成、温度和物态方程．如给定每一个重子的熵,一些热力学量的值将随重子密度的增加而增加,当考虑超子时,这些值会减小．给定重子密度,中子在S=2时的组分比S=1时的小,而质子、电子、μ子在S=2时的组分比S=1时的大,特别是在低密度区域．S是每个重子的熵．保持重子密度不变,在低密度区域,超子在S=2时的组分比S=1时的大,在高密度区域则相反．同样,在同一重子密度处,S=2时的温度、能量密度及压强分别比S=1时的大．另外,有限熵对粒子组分和温度的影响比对质子中子星物质的物态方程的影响大．还研究了反粒子的贡献,他们确实很小．