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
How and When Will a Neutron Star Become a Hyperon Star?
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
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.
JIA Huan-Yu;SUN Bao-Xi;MENG Jie;;ZHAO En-Guang. How and When Will a Neutron Star Become a Hyperon Star?[J]. 中国物理快报, 2001, 18(12): 1571-1574.
JIA Huan-Yu, SUN Bao-Xi, MENG Jie, , ZHAO En-Guang. How and When Will a Neutron Star Become a Hyperon Star?. Chin. Phys. Lett., 2001, 18(12): 1571-1574.
2001, Vol. 18 
