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How and When Will a Neutron Star Become a Hyperon Star? |
| JIA Huan-Yu1;SUN Bao-Xi2;MENG Jie1,2,3;ZHAO En-Guang2 |
| 1Department of Technical Physics, Peking University,
Beijing 100871
2Institute of Theoretical Physics, Chinese Academy of
Sciences, Beijing 100080
3Center of Theoretical Nuclear Physics, National Laboratory of Heavy Ion Accelerator, Lanzhou 730000 |
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| Cite this article: |
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JIA Huan-Yu, SUN Bao-Xi, MENG Jie et al 2001 Chin. Phys. Lett. 18 1571-1574 |
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Abstract In the framework of the extended relativistic mean-field theory with hyperons, the properties of neutron star matter have been investigated. It is found that at a density of four to five times of nuclear matter saturation density ρ0, a neutron star will become a hyperon star. This transition is strongly influenced by the coupling constants of hyperons to the mesons and different parameter set. For a given parameter set, a minimum transition baryon density exists when the hyperon coupling ratios satisfy xHσ = xHω = xHρ = 0.65 or xHσ = xHω = 0.62, xHρ = 0.7.
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| Keywords:
26.60.+c
21.60.-n
13.75.Ev
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Published: 01 December 2001
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