Multiple configurations of neutron stars containing quark matter  

作　　者：Wei Wei Shu-Hua Yang Ze-Han Bao Chong Zhang Chang Gao Wei-Ru Fan 魏薇;杨书华;鲍泽韩;张翀;高畅;樊玮茹(College of Science,HuaZhong Agricultural University,Wuhan 430070,China;College of Physical Science and Technology,Central China Normal University,Wuhan 430079,China)

机构地区：[1]College of Science,HuaZhong Agricultural University,Wuhan 430070,China [2]College of Physical Science and Technology,Central China Normal University,Wuhan 430079,China

出　　处：《Chinese Physics C》2020年第9期112-121,共10页中国物理C（英文版）

基　　金：Supported by National Natural Science Foundation of China(11903013)。

摘　　要：The main purpose of this study is to interpret the possibilities of hybrid star configurations under different phase transition paths and provide a general description of the conditions and features of the different configurations.We assume that there are two possible phase transition paths,i.e.,from a nuclear phase to a 2flavor(2f)/3flavor(3f)quark phase directly,or first from a nuclear phase to a 2f quark phase,and then from that phase to a 3f quark phase sequentially.In addition,we consider Maxwell and Gibbs constructions based on the assumption of a first-order transition,which yields multiple configurations of hybrid stars:N-2f,N-3f,and N-2f-3f for a Maxwell construction,and N-2fmix-2f,N-3fmix-3f,N-2f3fmix,and N-2fmix-3f for a Gibbs construction.From the radii analysis of different hybrid star configurations with the same mass of 1.95M⊙,the appearance of the quark matter(from nuclear to 2f or 3f quark matter)causes a radius difference of 0.5km^2km and provides the possibility of detection by NICER in the future.However,the sequential transition from 2f to 3f quark matter is difficult to detect because the transition does not lead to too high of a change in radius(far smaller than 0.5km).The dependence solely on the measurements of the stellar radii to probe the equation of state of dense matter in neutron stars causes difficulties.Multi-messenger observations can help us to infer the interior of a neutron star in the future.

关 键 词：neutron star deconfinement phase transition quark matter equation of state 

分 类 号：O571.5[理学—粒子物理与原子核物理]