标题： 核物质对于致密星体及其性质 显示英文标题

标题： Nuclear Matter for compact stars and its properties

摘要： 一种纯核子状态方程（EoS）用于β平衡电中性中子星（NS）物质，该EoS是通过密度依赖的有效NN相互作用确定的。 该EoS被发现满足从观测到的中子星质量-半径关系和重离子碰撞流数据得出的约束。 P. B. Demorest等人[1]对双星毫秒脉冲星J1614-2230的最新观测表明，质量位于(1.97\pm 0.04) M_\odot (M_\odot ，太阳质量)范围内。 大多数涉及奇异物质的状态方程，如介子凝聚或超子，往往预测的最大质量远低于2.0M_\odot ，因此被排除。 我们能够再现旋转和静态NS的测量质量-半径关系。 我们确保旋转速度不超过由r模式不稳定性限制的频率的恒星，其最大质量约为1.95M_\odot ，半径约为10公里。 显示英文摘要

摘要： A pure nucleonic equation of state (EoS) for beta equilibrated charge neutral neutron star (NS) matter is determined using density dependent effective NN interaction. This EoS is found to satisfy both the constraints from the observed mass-radius of neutron stars and flow data from heavy-ion collisions. Recent observations of the binary millisecond pulsar J1614-2230 by P. B. Demorest et al. [1] suggest that the masses lie within (1.97\pm 0.04) M_\odot (M_\odot, solar mass). Most EoS involving exotic matter, such as kaon condensates or hyperons, tend to predict maximum masses well below 2.0M_\odot and are therefore ruled out. We are able to reproduce the measured mass-radius relationship for rotating and static NS. We ensure that the star rotating not faster than the frequency limited by r-mode instability gives the maximum mass about 1.95M_\odot with radius about 10 kilometer.