Arxiv:2104.01524V2 [Nucl-Th] 6 May 2021 Μ Μ Sis
Quark stars in the pure pseudo-Wigner phase Li-Qun Su,1, ∗ Chao Shi,2,† Yong-Feng Huang,3,‡ Yan Yan,4,§ Cheng-Ming Li,5,¶ and Hongshi Zong1, 6, 7, 8, ∗∗ 1Department of physics, Nanjing University, Nanjing 210093, China 2Department of Nuclear Science and Technology, Nanjing University of Aeronautics and Astronautics, Nanjing 210016, China 3School of Astronomy and space science, Nanjing University, Nanjing 210023, China 4School of Mathematics and physics, Changzhou University,Changzhou 213164, China 5School of physics and Microelectronics, Zhengzhou University, Zhengzhou 450001, China 6Department of physics, Anhui Normal University, Wuhu 241000, China 7Nanjing Proton Source Research and Design Center, Nanjing 210093, China 8Joint Center for Particle, Nuclear Physics and Cosmology, Nanjing 210093, China (Dated: May 11, 2021) In this paper, the equation of state (EOS) of deconfined quark stars is studied in the framework of the two- flavor NJL model, and the self-consistent mean field approximation is employed by introducing a parameter a combining the original Lagrangian and the Fierz-transformed Lagrangian, LR = (1 − a)L + aLF , to measure the weights of different interaction channels. It is believed that the deconfinement of phase transition happens along with the chiral phase transition. Thus, due to the lack of description of confinement in the NJL model, the vacuum pressure is set to confine quarks at low densities, which is the pressure corresponding to the critical point of chiral phase transition. We find that deconfined quark stars can reach over two-solar-mass, and the bag constant therefore shifts from (130 MeV)4 to (150 MeV)4 as a grows.
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