论文标题
温暖的物质和超新星残留物的冷却
Warm dense matter and cooling of supernovae remnants
论文作者
论文摘要
我们使用NL3，G3和IU-FSU参数集对核物质（NM）特性（例如结合能，不可压缩能，自由对称能量及其系数）进行热效应。这些模型与冷NM的特性一致，也已通过纳入费米功能来研究温度的影响。对于对称NM中液体GAS相变的临界温度分别为14.60、15.37和14.50 MEV，分别为NL3，G3和IU-FSU参数集，这与以前的理论和实验研究非常吻合。我们检查，与饱和密度下的结合能的第二个差分系数和自由对称能有关（即k 0（n，t）和q sym，0），随着温度升高，NL3和G3参数的相反效果具有相反的效果。我们发现，在有限温度下，饱和曲率参数（k sym，0）的g3状态方程有利于k sym的组合分析，0对大量脉冲星的存在，GW170817的重力波以及PSR J0030+0451的重力波。此外，我们通过直接URCA过程控制的中微子发射率研究了新生恒星的冷却机制，并对中微子发射率进行了一些有趣的评论。我们还考虑温度对原始恒星的M-R轮廓的影响。
We study the thermal effects on the nuclear matter (NM) properties such as binding energy, incompressibility, free symmetry energy and its coefficients using NL3, G3 and IU-FSU parameter sets of relativistic mean-field models. These models being consistent with the properties of cold NM, have also been used to study the effect of temperature by incorporating the Fermi function. The critical temperature for the liquid-gas phase transition in the symmetric NM is found to be 14.60, 15.37 and 14.50 MeV for NL3, G3 and IU-FSU parameter sets respectively, which is in excellent agreement with previous theoretical and experimental studies. We inspect that the properties related to second differential coefficient of the binding energy and free symmetry energy at saturation density ( i.e. K 0 (n, T ) and Q sym,0) exhibit the contrary effects for NL3 and G3 parameters as the temperature increases. We find that the prediction of saturated curvature parameter ( K sym,0 ) for G3 equation of state at finite temperature favour the combined analysis of K sym,0 for the existence of massive pulsars, gravitational waves from GW170817 and NICER observations of PSR J0030+0451. Further, we investigate the cooling mechanism of newly born stars through neutrino emissivity controlled by direct Urca process and instate some interesting remarks about neutrino emissivity. We also deliberate the effect of temperature on the M-R profile of Proto-Neutron star.
