Kaon Condensation in Neutron Star Matter

GUO Hua; LIU Bo; LI Xi-Guo; CHEN Yan-Jun

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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(2) : 113-117

Kaon Condensation in Neutron Star Matter

Center of Nuclear Theoretical Physics,National Laboratory of Heavy Ion Accelerator of Lanzhou 730000,China2 Department of Technical Physics,and MOE Key Laboratory of Heavy Ion Physics,Peking University,Beijing 100871,China3 Institute of High Energy Physics,CAS,Beijing 100039,China4 Institute of Modern Physics,CAS,Lanzhou 730000,China

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Abstract：
The Kaon condensation in neutron star matter is calculated in the framework of the density dependent relativistic mean-field theory. The present results show that the critical density for the Kaon condensation is ～2.75ρ₀, while the critical densities for the URCA process in neutron star matter are ρρ0≈3.16 for the parameter set fitted to the DB nucleon self-energies of nuclear mater with the momentum-dependent correction, and ρρ0≈2.25 for the parameter set without the momentum-dependent correction. Then,influences of the two different model parameter sets on the equation of state of neutron star matter are discussed.

References

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GUO Hua, LIU Bo, LI Xi-Guo and CHEN Yan-Jun. Kaon Condensation in Neutron Star Matter[J]. Chinese Physics C, 2003, 27(2): 113-117.

GUO Hua, LIU Bo, LI Xi-Guo and CHEN Yan-Jun. Kaon Condensation in Neutron Star Matter[J]. Chinese Physics C, 2003, 27(2): 113-117. shu

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Received: 2002-03-21
Revised: 1900-01-01

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沈阳化工大学材料科学与工程学院沈阳 110142

Kaon Condensation in Neutron Star Matter

Corresponding author: GUO Hua,

Center of Nuclear Theoretical Physics,National Laboratory of Heavy Ion Accelerator of Lanzhou 730000,China2 Department of Technical Physics,and MOE Key Laboratory of Heavy Ion Physics,Peking University,Beijing 100871,China3 Institute of High Energy Physics,CAS,Beijing 100039,China4 Institute of Modern Physics,CAS,Lanzhou 730000,China

Received Date: 2002-03-21
Accepted Date: 1900-01-01
Available Online: 2003-02-05

Abstract: The Kaon condensation in neutron star matter is calculated in the framework of the density dependent relativistic mean-field theory. The present results show that the critical density for the Kaon condensation is ～2.75ρ₀, while the critical densities for the URCA process in neutron star matter are ρρ0≈3.16 for the parameter set fitted to the DB nucleon self-energies of nuclear mater with the momentum-dependent correction, and ρρ0≈2.25 for the parameter set without the momentum-dependent correction. Then,influences of the two different model parameter sets on the equation of state of neutron star matter are discussed.