Charged quark stars in f(R,T)gravity  

作　　者：Juan M.Z.Pretel Takol Tangphati Ayan Banerjee Anirudh Pradhan 

机构地区：[1]Centro Brasileiro de Pesquisas Físicas,Rua Dr.Xavier Sigaud,150 URCA,Rio de Janeiro CEP 22290-180,RJ,Brazil [2]Theoretical and Computational Physics Group,Theoretical and Computational Science Center(TaCS),Faculty of Science,King Mongkut’s University of Technology Thonburi,126 Prachauthid Rd.,Bangkok 10140,Thailand [3]Astrophysics and Cosmology Research Unit,School of Mathematics,Statistics and Computer Science,University of KwaZulu-Natal,Private Bag X54001,Durban 4000,South Africa [4]Centre for Cosmology,Astrophysics and Space Science,GLA University,Mathura-281406,Uttar Pradesh,India

出　　处：《Chinese Physics C》2022年第11期308-317,共10页中国物理C（英文版）

基　　金：financial support from the PCI program of the Brazilian agency"Conselho Nacional de Desenvolvimento Científico e Tecnológico"-CNPq;supported by King Mongkut's University of Technology Thonburi's Post-doctoral Fellowship。

摘　　要：Recent advances in nuclear theory and new astrophysical observations have led to the need for specific theoretical models applicable to dense-matter physics phenomena.Quantum chromodynamics(QCD)predicts the existence of non-nucleonic degrees of freedom at high densities in neutron-star matter,such as quark matter.Within a confining quark matter model,which consists of homogeneous,neutral 3-flavor interacting quark matter with O(m_(s)^(4))corrections,we examine the structure of compact stars composed of a charged perfect fluid in the context of f(R,T)gravity.The system of differential equations describing the structure of charged compact stars has been derived and numerically solved for a gravity model with f(R,T)=R+2βT.For simplicity,we assumed that the charge density is proportional to the energy density,namely,ρ_(ch)=αρ.It is demonstrated that the matter-geometry coupling constant β and charge parameter α affect the total gravitational mass and the radius of the star.

关 键 词：charged stars f(R T)gravity 

分 类 号：P14[天文地球—天体物理]