混杂星的r-模不稳定性窗口  

The R-Mode Instability Window of the Hybrid Stars

作　　者：潘娜娜[1] 杨书华[1] 郑小平[1] 

机构地区：[1]华中师范大学物理科学与技术学院,武汉430079

出　　处：《天文学报》2004年第3期272-278,共7页Acta Astronomica Sinica

基　　金：国家自然科学基金(10373007)资助项目

摘　　要：考虑到混杂星既具有奇异夸克物质核,又具有中子星固体壳层的特殊结构,运用完全自洽的二级修正方法,研究了在低温极限下(T<109K)混杂星的体粘滞耗散时标,并利用该时标计算了混杂星的临界旋转频率,发现其最小值为704.42 Hz(对应1.42 ms脉冲周期).与中子星和奇异星比较,更好地解释了观测数据.The hybrid star contains both a strange quark matter core and a solid crust of the neutron star. Considering this kind of particular structure, we utilize the fully self-consistent second-order correction technique to estimate the bulk viscosity damping timescale of the hybrid star at low temperature (T < 109 K), as well as the critical spin frequency which bases on the timescale. Compared with the neutron star and the strange star, we find that its minimum frequency rises to 704.42 Hz (that is 1.42ms pulsar period),which can explain the observed data better.

关 键 词：混杂星 夸克物质核 中子星 脉冲周期 致密物质 引力 恒星 振荡 

分 类 号：P152[天文地球—天文学]