Sound velocity in dense stellar matter with strangeness and compact stars  

作　　者：Chengjun Xia Zhenyu Zhu Xia Zhou Ang Li 夏铖君;朱镇宇;周霞;李昂(School of Information Science and Engineering,Zhejiang University Ningbo Institute of Technology.Ningbo 315100 China;Department of Astronomy,Xiamen University,Xiamen 361005,China;Xinjiang Astronomical Observatory,Chinese Academy of Sciences,Urumqi 830011,China)

机构地区：[1]School of Information Science and Engineering,Zhejiang University Ningbo Institute of Technology.Ningbo 315100 China [2]Department of Astronomy,Xiamen University,Xiamen 361005,China [3]Xinjiang Astronomical Observatory,Chinese Academy of Sciences,Urumqi 830011,China

出　　处：《Chinese Physics C》2021年第5期237-246,共10页中国物理C（英文版）

基　　金：National SKA Program of China(2020SKA0120300);the National Natural Science Foundation of China(11873040);the Youth Innovation Fund of Xiamen(3502Z20206061).Ningbo Natural Science Foundation(2019A610066);CAS"Light of West China"Program(2018-XBQNXZ-B-025);Tianshan Youth Program(2018Q039)。

摘　　要：The phase state of dense matter in the intermediate density range(~1-10 times the nuclear saturation density)is both intriguing and unclear and can have important observable effects in the present gravitational wave era of neutron stars.As matter density increases in compact stars,the sound velocity is expected to approach the con-formal limit(cs/c=1/√3)at high densities and should also fulfill the causality limit(cs/c<1).However,its de-tailed behavior remains a prominent topic of debate.It was suggested that the sound velocity of dense matter could be an important indicator of a deconfinement phase transition,where a particular shape might be expected for its density dependence.In this work,we explore the general properties of the sound velocity and the adiabatic index of dense matter in hybrid stars as well as in neutron stars and quark stars.Various conditions are employed for the had-ron-quark phase transition with varying interface tension.We find that the expected behavior of the sound velocity can also be achieved by the nonperturbative properties of the quark phase,in addition to a deconfinement phase transition.Moreover,it leads to a more compact star with a similar mass.We then propose a new class of quark star equation of states,which can be tested by future high-precision radius measurements of pulsar-like objects.

关 键 词：quark matter hadron-quark phase transition neutron star 

分 类 号：P144[天文地球—天体物理]