Neutron star cooling and GW170817 constraint within quark-meson coupling models  

作　　者：Odilon Lourenço César H.Lenzi Mariana Dutra Tobias Frederico M.Bhuyan Rodrigo Negreiros César V.Flores Guilherme Grams Débora P.Menezes 

机构地区：[1]Departamento de Física,Instituto Tecnológico de Aeronáutica,DCTA,12228-900,São Josédos Campos,SP,Brazil [2]Department of Physics,Faculty of Science,University of Malaya,Kuala Lumpur 50603,Malaysia [3]Atomic Molecular and Optical Research Group,Advanced Institute of Materials Science,Ton Duc Thang University,Ho Chi Minh City,Vietnam [4]Faculty of Applied Sciences,Ton Duc Thang University,Ho Chi Minh City,Vietnam [5]Instituto de Física,Universidade Federal Fluminense 20420,Niterói,RJ,Brazil [6]Centro de Ciências Exatas,Naturais e Tecnológicas,UEMASUL,Rua Godofredo Viana 1300,Centro CEP:65901-480,Imperatriz,Maranhão,Brazil [7]Departamento de Física,Universidade Federal de Santa Catarina,Florianópolis,SC,CP 476,CEP 88.040-900,Brazil [8]Univ.Lyon,Univ.Claude Bernard Lyon 1,CNRS/IN2P3,IP2I Lyon,UMR 5822,F-69622,Villeurbanne,France

出　　处：《Chinese Physics C》2021年第2期531-547,共17页中国物理C（英文版）

基　　金：This work is a part of the projet INCT-FNA Proe.(464898/2014-5),was partially supprted by CNPq(Brazil)(301155.2017-8)(D.P.M.),310242/2017-7,406958/2018-1(O.L),308486/2015-3(T.F.),43369/2018-3(M.D.),by Capes-PNPD program(C.V.F),and by Fundacio de Amparo a Pesquisa do Estado de Sio Paulo(FAPESP)under the thematic projescts 2013/26258-4(OL,TF)and 2017/05660-0(OL,M.D.T.E.).R.N.also acknowledges that this project was parly funded by FAPERJ,under grant E-26/203.2992017.M.B.acknowledge the support from FAPESP Project No.2017/05660-0,and FOSTECT Project No.FOSTECT.2019B.04.PDS acknow ledges support from the UK STFC under projeet number ST/P005314/1。

摘　　要：In the present work,we used five different versions of the quark-meson coupling(QMC)model to compute astrophysical quantities related to the GW170817 event and the neutron star cooling process.Two of the models are based on the original bag potential structure and three versions consider a harmonic oscillator potential to confine quarks.The bag-like models also incorporate the pasta phase used to describe the inner crust of neutron stars.With a simple method studied in the present work,we show that the pasta phase does not play a significant role.Moreover,the QMC model that satisfies the GW170817 constraints with the lowest slope of the symmetry energy exhibits a cooling profile compatible with observational data.

关 键 词：equation of state compact star cooling in stars quark-meson coupling models tidal deformability neutron star merger 

分 类 号：P145.6[天文地球—天体物理]