Condensations of K<SUP>－</SUP> and K<SUP>0</SUP> in Neutron Star Matter

DING Wen-Bo; LIU Guang-Zhou

Chinese Physics C> 2006, Vol. 30> Issue(S2) : 249-251

Condensations of K^－ and K⁰ in Neutron Star Matter

DING Wen-Bo ^, ,
LIU Guang-Zhou

Center for Theoretical Physics, Jilin University, Changchun 130023, China

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Abstract：
In the framework of the relativistic mean field theory(RMFT),the condensations of K^－ and K⁰ in neutron star matter are studied. We find that K^－ and K⁰ condensations can both occur,even in the case that the neutron star matter includes baryon octet and Δ resonances.Also we investigate how hyperons and K condensations influence each other. K⁰ condensations depress K^－ condensations and make Δ resonances appear easily. In the high density region, the system may consist of many kinds of baryons, whose number densities are becomming identical. And ultimately K⁰-rich matter is formed in the core. The equation of state including K condensations becomes softer resulting in a smaller maximum mass of neutron star.

References

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DING Wen-Bo and LIU Guang-Zhou. Condensations of K^－ and K⁰ in Neutron Star Matter[J]. Chinese Physics C, 2006, 30(S2): 249-251.

DING Wen-Bo and LIU Guang-Zhou. Condensations of K^－ and K⁰ in Neutron Star Matter[J]. Chinese Physics C, 2006, 30(S2): 249-251. shu

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Received: 2006-10-18
Revised: 1900-01-01

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通讯作者: 陈斌, bchen63@163.com

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沈阳化工大学材料科学与工程学院沈阳 110142

Condensations of K^－ and K⁰ in Neutron Star Matter

Corresponding author: DING Wen-Bo,

Center for Theoretical Physics, Jilin University, Changchun 130023, China

Received Date: 2006-10-18

Accepted Date: 1900-01-01

Available Online: 2006-01-03

Abstract: In the framework of the relativistic mean field theory(RMFT),the condensations of K^－ and K⁰ in neutron star matter are studied. We find that K^－ and K⁰ condensations can both occur,even in the case that the neutron star matter includes baryon octet and Δ resonances.Also we investigate how hyperons and K condensations influence each other. K⁰ condensations depress K^－ condensations and make Δ resonances appear easily. In the high density region, the system may consist of many kinds of baryons, whose number densities are becomming identical. And ultimately K⁰-rich matter is formed in the core. The equation of state including K condensations becomes softer resulting in a smaller maximum mass of neutron star.

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Condensations of K^－ and K⁰ in Neutron Star Matter

Condensations of K^－ and K⁰ in Neutron Star Matter