Can the Moment of Inertia of Massive Neutron Stars be Used to Constrain the Hyperon Couplings?

YU Zi; DING Wenbo; XU Yan; ZHANG Guiqing

doi:10.11804/NuclPhysRev.35.02.127

In the framework of the relativistic mean field theory(RMFT) with GL91 cets, the momentum of inertia (I) of slowly rotating neutron stars is studied by perturbative approach. The scalar hyperon coupling should lie in the range of X_σ=0.59~1.0 to be compatible with massive neutron stars. As X_σ increases from 0.59 to 1.0, the maximum momentum of inertia(I_max) of neutron (protoneutron) stars increases by 89% (60%). According to the data of Crab, the maximum energy loss(dE/dt) of neutron (protoneutron) stars will increase by 44%(25%)and the maximum magnetic field (B) will increase by 48%(38%). I and dE/dt of PSR J0348+0432 both increase by 14%, while B decreases by 10% as X_σ increases from 0.59 to 1.0. So if the upper bound of I, or the accurate values of both the mass and I of neutron stars could be provided by the astronomical observations, the hyperon couplings should be further constrained in the future.

Can the Moment of Inertia of Massive Neutron Stars be Used to Constrain the Hyperon Couplings?

1. College of science, Nanjing Forestry University, Nanjing 210037, China;

2. Physics Department of Bohai University, Jinzhou 121013, LIASOning, China;

3. Changchun Observatory, National Astronomical Observatories, Chinese Academy of Sciences, Changchun 130117, China;

4. Department of Physics, Tianjing University of Science and Technology, Tianjing 300457, China

Funds: Natural Science Fundamental Research Project of Jiangsu Colleges and Universities (Bk20140982); National Natural Science Foundation of China (11265009, 11175077, 11271055)

Received Date: 2018-04-20

Rev Recd Date: 2018-05-26

Publish Date: 2018-06-20

Key words:

Abstract: In the framework of the relativistic mean field theory(RMFT) with GL91 cets, the momentum of inertia (I) of slowly rotating neutron stars is studied by perturbative approach. The scalar hyperon coupling should lie in the range of X_σ=0.59~1.0 to be compatible with massive neutron stars. As X_σ increases from 0.59 to 1.0, the maximum momentum of inertia(I_max) of neutron (protoneutron) stars increases by 89% (60%). According to the data of Crab, the maximum energy loss(dE/dt) of neutron (protoneutron) stars will increase by 44%(25%)and the maximum magnetic field (B) will increase by 48%(38%). I and dE/dt of PSR J0348+0432 both increase by 14%, while B decreases by 10% as X_σ increases from 0.59 to 1.0. So if the upper bound of I, or the accurate values of both the mass and I of neutron stars could be provided by the astronomical observations, the hyperon couplings should be further constrained in the future.

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Reference (21)

[1]	BETHE H A. Rev Mod Phys, 1990, 62:801.
[2]	GLENDENNING N K. Compact stars:Nuclear Physics, Particle Ph and General Relativity[M]. New York:Springer:1997:206.
[3]	DEMOREST P B, PENNUCCI T, RANSOM S M, et al. Nature, 2010, 467:1081.
[4]	ANTONIADIS J, WHELAN D G. Science, 2013, 340(6131):448.
[5]	LI T P, XIONG S L, ZHANG S N, et al. Science China Physics Mechanics & Astronomy, 2018, 61:031011.
[6]	ABBOTT B P, et al. Phys Rev Lett, 2017, 119:161101.
[7]	JIANG W Z, LI B A, CHEN L W. Astrophys J, 2012, 756:56.
[8]	HARTLE J B. Astrophysics & Space Science, 1973, 24:385.
[9]	FATTOYEV F J, PIEKAREWICZ J. Phys Rev C, 2010, 82:025810.
[10]	HONG B, JIA H Y, MU X L, et al. Chin Phys C, 2016, 40:35.
[11]	ZHAO X F, JIA H Y. Journal of Astrophysics & Astronomy, 2012, 33:303.
[12]	DATTA B, RAY A. Monthly Notices of the Royal Astronomical Society, 1983, 204:75.
[13]	ZHAO Xianfeng, WANG Shunjing, ZHANG Hua, et al. Journal of Sichuan University(Natural Science Edition), 2009, 46(3):743. (in Chinese) (赵先锋, 王顺金, 张华, 等. 四川大学学报:自然科学版, 2009, 46(3):743.)
[14]	ZHAO Xianfeng, WANG Shunjing, ZHANG Hua, et al. Journal of Southwest University(Natural Science Edition), 2010, 32(7):46. (in Chinese) (赵先锋, 王顺金, 张华, 等. 西南大学学报(自然科学版), 2010, 32(7):46.)
[15]	ZHAO Xianfeng. Acta Astronomic Sinica, 2011, 52(2):126. (in Chinese) (赵先锋. 天文学报, 2011, 52(2):126.)
[16]	HEWISH A, OKOYE S E. Nature, 1964, 203:171
[17]	GLENDENNING N K, MOSZKOWSKI S A. Phys Rev Lett, 1991, 67:2414.
[18]	SCHAFFNER J, MISHUSTIN I N. Phys Rev C, 1996, 53:1416.
[19]	SCHAFFNER J, DOVER C B, GAL A, et al. Annals Phys, 1994, 235:35.
[20]	YANG F. SHEN H. Phys Rev C, 2008, 77:025801.
[21]	PACINI F. Nature, 1968, 219:45.

Can the Moment of Inertia of Massive Neutron Stars be Used to Constrain the Hyperon Couplings?

doi: 10.11804/NuclPhysRev.35.02.127

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