Key factor for determining relation between radius and tidal deformability of neutron stars: Slope of symmetry energy  

作　　者：Nai-Bo Zhang Bin Qi Shou-Yu Wang 张乃波;亓斌;王守宇(Shandong Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment,School of Space Science and Physics,Institute of Space Sciences,Shandong University,Weihai 264209,China)

机构地区：[1]Shandong Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment,School of Space Science and Physics,Institute of Space Sciences,Shandong University,Weihai 264209,China

出　　处：《Chinese Physics C》2020年第6期103-108,共6页中国物理C（英文版）

基　　金：This work is partly Supported by the Shandong Natural Science Foundation(JQ201701);the Natural Science Foundation of China(11622540,11675094,11705102,11775133);the China Postdoctoral Science Foundation(2019M652358);the Young Scholars Program of Shandong University,Weihai(2015WHWLJH01);the Fundamental Research Funds of Shandong University(2019ZRJC001)。

摘　　要：The constraints on tidal deformability Λ of neutron stars were first extracted from GW170817 by LIGO and Virgo Collaborations.However,the relationship between the radius R and tidal deformability Λ is still under debate.Using an isospin-dependent parameterized equation of state(EOS),we study the relation between R andΛand its dependence on parameters of symmetry energy Esym and EOS of symmetric nuclear matter E0 when the mass is fixed at 1.4 M⊙,1.0 M⊙,and 1.8 M⊙.We find that,although the changes of high order parameters of Esym and E 0 can shift individual values of R1.4 and Λ1.4,the R1.4~Λ1.4 relation remains approximately at the same fitted curve.The slope L of the symmetry energy plays the dominant role in determining the R1.4~Λ1.4 relation.By investigating the mass dependence of the R~Λ relation,we find that the well fitted R~Λ relation for 1.4 M⊙ is broken for massive neutron stars.

关 键 词：neutron stars symmetry energy tidal deformability RADIUS 

分 类 号：P145.6[天文地球—天体物理]