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《中国物理C》（英文）编辑部
2024年10月30日
Chinese Physics C> 2003, Vol. 27> Issue(3) : 200-205 

Effect of Temperature on Hyperon Neutron Star

  •  College of Science, Southwest Jiaotong University, Chengdu 610031, China2 Department of Technical Physics, Peking University, Beijing 100871, China3 Institute of Theoretical Physics, Chinese Academy of Science, Beijing 100080, China4 Center of Theoretical Nuclear Physics, National Laboratory of Heavy Ion Accelerator, Lanzhou 730000, China5 Department of Physics, Wuhan University, Wuhan 430072, China

  • The influences of temperature on the constitutes, equations of state and masses of neutron star are studied in the frame work of the relativistic mean field theory for an interacting nucleons, hyperons, and mesons system. It is found that the appearing density of hyperons becomes smaller with temperature increasing. At higher hadron densities, the core of the neutron star is dominated by hyperons, in another words a neutron star transits into a hyperon star. The effects of temperature on the transition of a neutron star to a hyperon star are also investigated. The higher the temperature is, the smaller the transition density is. And it is also found that the equations of state for hadronic matter in the core region of a neutron star are approximately the same at different temperature. The calculated maximum masses of neutron stars are about 1.8M⊙, which are in consistence with the observation.
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    [1] . Burrows A ,Lattimer J M .Astrophy.J .,1986,307:1862. Lattimer J M ,Pethick C J ,Prakash M et al.Phys.Rev.Lett.,1991,66:27013. Cooperstein J, Baron E .Supernova,Ed.Petschek A G .,Springer Verlog,1990,P2134. Bethe H A .Nucl.Phys.,1979,A324:4875. Lamb D Q et al.Phys.Rev.Lett.,1978,41:16236. Lattimer J M et al.Nucl.Phys.,1985,A432:6467. Swesty F D ,Lattimer J M ,Myra E S .Ap.J.,1994,425:1958. Prakash M et al.Phys.Rep.,1997,280:19. Manka R et al.Phys.Rev.,2000,C62:01580210. Cameron A G W .Ap.J.,1959,130:88411. Ambartsumyan V A ,Saakyan G S .Astron.Zh.,1963,37:19312. Pandharipande V R .Nucl.Phys.,1971,A178:12313. Bethe H A ,Johnson M .Nucl.Phys.,1974,A230:114. Glendenning N K .Phys.Lett.,1982,B114:39215. Glendenning N K .Z .Phys.,1987,A326:5716. Glendenning N K .Nucl.Phys.,1989,A493:52117. Ellis J,Kapusta J I,Olive K A .Nucl.Phys.,1991,B348:34518. Kapusta J I,Olive K A .Phys.Rev.Lett.,1990,64:1319. Glendning N K .Phys.Lett.,1987,B185:27520. Glendenning N K .Nucl.Phys.,1987,A469:60021. Glendenning N K .Ap.J.,1985,293:47022. Glendenning N K ,Moszkowski S A .Phys.Rev.Lett.,1991,67:241423. Schaffner J,Greiner C ,Stocker H .Phys.Rev.,1992,C46:32224. Schaffner J et al.Phys.Rev.Lett.,1993,71:132825. Schaffner J et al.Ann.Phys.(N .Y .),1994,235:35

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JIA Huan-Yu, MENG Jie, ZHAO En-Guang, LI Jun and SANG Jian-Ping. Effect of Temperature on Hyperon Neutron Star[J]. Chinese Physics C, 2003, 27(3): 200-205.
JIA Huan-Yu, MENG Jie, ZHAO En-Guang, LI Jun and SANG Jian-Ping. Effect of Temperature on Hyperon Neutron Star[J]. Chinese Physics C, 2003, 27(3): 200-205. shu
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Received: 2002-03-20
Revised: 1900-01-01
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Effect of Temperature on Hyperon Neutron Star

    Corresponding author: JIA Huan-Yu,
  • College of Science, Southwest Jiaotong University, Chengdu 610031, China2 Department of Technical Physics, Peking University, Beijing 100871, China3 Institute of Theoretical Physics, Chinese Academy of Science, Beijing 100080, China4 Center of Theoretical Nuclear Physics, National Laboratory of Heavy Ion Accelerator, Lanzhou 730000, China5 Department of Physics, Wuhan University, Wuhan 430072, China
  • Received Date: 2002-03-20
  • Accepted Date: 1900-01-01
  • Available Online: 2003-03-05

Abstract: The influences of temperature on the constitutes, equations of state and masses of neutron star are studied in the frame work of the relativistic mean field theory for an interacting nucleons, hyperons, and mesons system. It is found that the appearing density of hyperons becomes smaller with temperature increasing. At higher hadron densities, the core of the neutron star is dominated by hyperons, in another words a neutron star transits into a hyperon star. The effects of temperature on the transition of a neutron star to a hyperon star are also investigated. The higher the temperature is, the smaller the transition density is. And it is also found that the equations of state for hadronic matter in the core region of a neutron star are approximately the same at different temperature. The calculated maximum masses of neutron stars are about 1.8M⊙, which are in consistence with the observation.

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