Hadron-Quark Mixed Stars Containing Fermion Dark Matter

LI Li; Tmurbagan; Baigala; LIU Guangzhou

doi:10.11804/NuclPhysRev.35.04.561

The observational properties of quark core hybrid star contain dark matter are studied. The influences of containing of strongly or weakly interacting dark matter to global observational features of hybrid stars, mass, radius, gravitational red-shift, rotational period and moment of inertia are studied by using relativistic mean field theory to describe hadron phase, effective mass bag model to quark phase, and Gibbs phase equilibrium conditions to hadron-quark mixed phase respectively. Our results indicate that, both in the strong and weak interacting case, the equation of state for hybrid star matter contain dark matter become softer than that of without dark matter while the mass of dark matter particles larger than 0.5 GeV, which leads to the decrease of the mass and corresponding radius of hybrid star. With the increase of the dark matter particle mass, the equation of state for hybrid star matter become softer, this cause the decrease of the mass and radius of hybrid star obviously. The gravitational red-shift and the rotational period, obviously increase of the moment of inertia of the hybrid stars are influenced by the dark matter particle mass. When the dark matter particle mass is equal to 0.1 GeV, the masses of the star with strong and weak interacting dark matter reach to 2.0 M_⊙ and 2.8 M_⊙(M_⊙ is the solar mass), this result indicates that the giant mass PSR, J1859-0131 and J1931-01, can be a hadron-quark hybrid star and containing dark matter with small dark particle mass. The computational results of all above global observational features of hybrid stars are in the range of astronomical observation data, these also indicate that hybrid star with quark core may contains dark matter.

Hadron-Quark Mixed Stars Containing Fermion Dark Matter

1. Institute of Physics and Electronics Information, Inner Mongolia University for the Nationalities, Tong Liao 028043, Inner Mongolia, China;

2. Center for Theoretical Physics, Jilin University, Changchun 130023, China

Funds: National Natural Science Foundation of China(11265009, 11075063); Science Foundation of Inner Mongolia University for Nationalities(NMDBS275)

Received Date: 2018-09-14

Rev Recd Date: 2018-11-11

Publish Date: 2020-05-03

Key words:

Abstract: The observational properties of quark core hybrid star contain dark matter are studied. The influences of containing of strongly or weakly interacting dark matter to global observational features of hybrid stars, mass, radius, gravitational red-shift, rotational period and moment of inertia are studied by using relativistic mean field theory to describe hadron phase, effective mass bag model to quark phase, and Gibbs phase equilibrium conditions to hadron-quark mixed phase respectively. Our results indicate that, both in the strong and weak interacting case, the equation of state for hybrid star matter contain dark matter become softer than that of without dark matter while the mass of dark matter particles larger than 0.5 GeV, which leads to the decrease of the mass and corresponding radius of hybrid star. With the increase of the dark matter particle mass, the equation of state for hybrid star matter become softer, this cause the decrease of the mass and radius of hybrid star obviously. The gravitational red-shift and the rotational period, obviously increase of the moment of inertia of the hybrid stars are influenced by the dark matter particle mass. When the dark matter particle mass is equal to 0.1 GeV, the masses of the star with strong and weak interacting dark matter reach to 2.0 M_⊙ and 2.8 M_⊙(M_⊙ is the solar mass), this result indicates that the giant mass PSR, J1859-0131 and J1931-01, can be a hadron-quark hybrid star and containing dark matter with small dark particle mass. The computational results of all above global observational features of hybrid stars are in the range of astronomical observation data, these also indicate that hybrid star with quark core may contains dark matter.

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Reference (17)

[1]	TMURBAGEN, DING Wenbo. Phase Structure of Neutron Star Equation of State[M]. Chifeng:Inner Mongolia Science and Technology Press, 2013:1. (in Chinese) (特木尔巴根, 丁文波. 子星状态方程相结构[M]. 赤峰:内蒙古科学技术出版社, 2013:1.)
[2]	BOGUTA J. Phys Lett B, 1981, 106(4):255.
[3]	GLEDENNING N K, SCHAFFNER J. Phys Rev C, 1999, 60(2):025803.
[4]	THORSETT S E, CHAKRABARTY D. The Astrophysical Journal, 1999, 512(1):288.
[5]	BAO Tmurbagen, TANG Gaowa. Journal of Nanyang Teachers College, 2009, 8(3):36. (in Chinese) (包特木尔巴根, 唐高娃. 南阳师范学院学报, 2009, 8(3):36.)
[6]	SCHFFNER J, MISHUSTIN I N. Phys Rev C, 1996, 53(3):1416.
[7]	BAO Tmurbagan, LIU Guangzhou, ZHU Mingfeng, et al. Commun Theor Phys, 2006, 45:505.
[8]	PEREZ-GARCIA M A, SILK J, STONE J R. Phys Rev Lett, 2010, 105(14):141101.
[9]	LEUNG S C, CHU M C, LIN L M. Phys Rev D, 2012, 85(10):471.
[10]	LI A, PENG G X, LU J F. RAA, 2011, 11(4):482.
[11]	BI Xiaojun, QIN Bo. Physical, 2011, 40(1):13. (in Chinese) (毕效军, 秦波. 物理, 2011, 40(1):13.)
[12]	YUAN Xuecheng, GENG Shufang, JIANG Mei. Acta geo Sinica, 2015, 89(12):2213. (袁学诚, 耿树方, 姜枚. 地质学报, 2015, 89(12):2213.)
[13]	CHANG Jin. Engineering Research-Interdisciplinary Perspectives, 2010, 2(2):95. (in Chinese) (常进. 工程研究-跨学科视野中的工程, 2010, 2(2):95.)
[14]	LI A, HUANG F, XU R X. Astroparticle Physics, 2012, 37(3):70.
[15]	RAIN G N, SCHAFFNER-BIELICH J, MISHUSTIN I N. Phys Rev D, 2006, 74(6):247.
[16]	GOLDMAN I, NUSSINOV S. Phys Rev D, 1989, 40:3221.
[17]	KOUVARIS C. Phys Rev D, 2008, 77:023006.

Hadron-Quark Mixed Stars Containing Fermion Dark Matter

doi: 10.11804/NuclPhysRev.35.04.561

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