中文摘要：

考虑到矿，中介子的贡献及重子八重态{n，p，∧，∑^-，∑^0，∑^＋，≡^-，≡^0}，采用相对论平均场方法，在5—25MeV的有限温度范围内，对中子星物质的性质进行了研究．发现当考虑到σ^＊，Ф介子的贡献后，超子出现的临界密度降低了（但对∧超子，影响并不显著），超子的粒子数密度增加了，在能量密度较高时物态方程变软，中子星的最大质量变小而相应的半径增大，中子星的中心粒子数密度、中心能量密度和中心压强都降低了．当温度为较低的T=5MeV，10MeV时，σ^＊，Ф介子的参与使出现∑^0，≡^0，∑^＋超子的临界密度极大地降低了；但当温度为较高的T=15MeV，20MeV，25MeV时，影响则较小．对于∧，∑^-，≡^-超子来说，在上述所有温度下，矿，中介子对超子出现的临界密度的影响都不明显．

英文摘要：

Within the RMF approach, considering the contribution of σ^＊, Ф mesons and baryon octet {n,p, ∧, ∑, E^-, ∑^0. ∑^＋,≡^-,≡^0, some properties of neutron star matter have been investigated in the temperature region between 5-15MeV. It is found that when the contributions of σ＊, Ф mesons are included, （1） the critical baryon density decreases （but for the A hyperon, the effect is not obvious）, but the number of hyperons increases; （2） the equation of state becomes soft at higher energy density; （3） the maximum mass decreases while the corresponding radius increases; （4） the central density, the central energy density, and the central pressure all become smaller. At T=5MeV and 10MeV and for ∑^0,≡^0,∑^＋, the σ＊, Ф mesons make critical baryon density greatly decrease; but at T=15MeV, 20MeV, and 25MeV, the effect is not obvious. However, for ∧, ∑^-, ≡^- hyperons, at all the above temperatures, the effect is not obvious.