中子星内部结构  

The inner structure of neutron stars

作　　者：来小禹 徐仁新[2] LAI Xiao-Yu;XU Ren-Xin(School of Physics and Engineering,Hubei University of Education,Wuhan 430205,China;School of Physics,Peking University,Beijing 100871,China)

机构地区：[1]湖北第二师范学院物理与机电工程学院,武汉430205 [2]北京大学物理学院,北京100871

出　　处：《物理》2019年第9期554-560,共7页Physics

基　　金：国家自然科学基金(U1831104,11673002)资助项目

摘　　要：中子星是宇宙中一类极端致密的天体,其平均密度超过饱和核物质密度。对这类天体的研究,可以帮助人们了解极端条件下的物理性质,特别是深化关于引力和强力的认识。文章介绍了脉冲星和中子星的概念,并重点阐述了中子星内部结构的不同模型,以及如何通过最大质量和潮汐形变量等观测来检验这些模型。未来发现更多的双中子星并合或中子星黑洞并合事件,有望最终揭开中子星内部结构之谜。Neutron stars are extremely compact objects with an average density higher than that o f the saturate nuclear matter. Exploring the nature o f such objects can help us to understand physics under extreme conditions, especially the gravitational and strong forces. This paper introduces the concepts o f pulsars and neutron stars, as well as various models o f the interior structure o f the latter. M ore importantly, we shall show how to test such models observationally by determining various properties related to the equation o f state, such us the maxim um mass and tidal deformability. Detecting further merger events o f binary neutron stars and/or neutron star-black hole binaries w ill certainly help to unveil the inner structure o f neutron stars.

关 键 词：中子星 脉冲星 引力波 致密物态 伽马射线暴 

分 类 号：P145.6[天文地球—天体物理]