Properties of hybrid stars in an extended MIT bag model

The properties of hybrid stars are investigated in the framework of the relativistic mean field theory （RMFT） and an MIT bag model with density-dependent bag constant to describe the hadron phase （HP） and quark phase （QP）, respectively. We find that the density-dependent B（p） decreases with baryon density p; this decrement makes the strange quark matter become more energetically favorable than ever, which makes the threshold densities of the hadron-quark phase transition lower than those of the original bag constant case. In this case, the hyperon degrees of freedom can not be considered. As a result, the equations of state of a star in the mixed phase （MP） become softer whereas those in the QP become stiffer, and the radii of the star obviously decrease. This indicates that the extended MIT bag model is more suitable to describe hybrid stars with small radii.     

K0 Condensation in Hyperonic Neutron Star Matter

In the framework of the relativistic mean field theory, we investigate K^0 condensation along with K^- condensation in neutron star matter including the baryon octet. The results show that both K^0 and K^- condensations can occur well in the core of the maximum mass stars for relatively shallow optical potentials of K^- in the range of-100 MeV～ -160 MeV. With the increasing optical potential of K^-, the critical densities of K^- decrease and the species of baryons appearing in neutron stars become fewer. The main role of K^0 condensation is to make the abundances of particles become identical leading to isospin saturated symmetric matter including antikaons, nucleons and hyperons. K^- condensation is chiefly responsible for the softening of the corresponding equation of state, which leads to a large reduction in the maximum masses of neutron stars. In the core of massive neutron stars, neutron star matter including rich particle species, such as antikaons, nucleons and hyperons, may exist.     

奇异物质体黏滞系数的计算和奇异星振动的阻尼

利用与奇异夸克质量相关的非轻子弱过程u+s←→d+u的反应速率, 在考虑了夸克之间的相互作用并做了热力学自恰处理后, 重新推导、计算了奇异夸克物质的体黏滞系数. 由于热力学自恰的需要引入一项压力附加项, 使得奇异星的体黏滞系数比前人计算的有了很大的增加. 通过计算振动衰减时间我们发现, 虽然体黏滞系数增大了很多, 但以前对于奇异星观测的结论仍然成立.     

热力学自洽的质量密度依赖夸克模型与混合星

用热力学自洽的质量密度依赖夸克模型描述夸克物质研究了混合星的基本性质, 计算了混合星内粒子分布、状态方程和对应的质量-半径关系. 结果表明, 质量密度依赖夸克模型中由热力学自洽处理所引起的压强附加项使整个混合星的状态方程变软, 相变始末点推迟, 从而使混合星的最大质量由无附加项时的大于2.4M_⊙, 变到小于1.8M_⊙, 相应的半径R由大于15km变到小于12.0km. 与NJL模型类似, 该模型更适合描述大质量的混合星.