The equation of state at finite temperature: Structure and composition of protoneutron stars

6th Nuclear Physics in Astrophysics

物理学;天文学

Burgio, G.F.^1 ; Baldo, M.^1 ; Chen, H.^2 ; Schulze, H.-J.^1

INFN Sezione di Catania, Via S. Sofia 64, Catania

95123, Italy^1

Department of Physics, China University of Geoscience, Wuhan

430074, China^2

关键词: Brueckner-Hartree-Fock approach;    Equation of state;    Finite temperatures;    Hadronic matters;    Quark matter;    Quark model;    Solar mass;    Three-body force;   

Others  :  https://iopscience.iop.org/article/10.1088/1742-6596/665/1/012062/pdf
DOI  :  10.1088/1742-6596/665/1/012062

学科分类：天文学(综合)

来源: IOP

【 摘 要 】

We study the hadron-quark phase transition at finite temperature in the interior of protoneutron stars, combining the equation of state obtained within the Brueckner-Hartree-Fock approach for hadronic matter with the MIT bag and the Dyson-Schwinger models for quark matter. We discuss the dependence of the results on different nuclear three-body forces and on details of the quark model. We find that a maximum mass exceeding two solar masses can be obtained with a strong three-body force and suitable parameter values in the Dyson-Schwinger model.