中国物理B ›› 2007, Vol. 16 ›› Issue (7): 1934-1940.doi: 10.1088/1009-1963/16/7/021

• • 上一篇    下一篇

Hyperon--hyperon interaction in relativistic mean field model

BurgioG1, 李昂2, 左维2, 米爱军3   

  1. (1)INFN Sezione di Catania, Via Santa Sofia 64, I- 95123 Catania, Italy 060853; (2)Institute of Modern Physics, Chinese Academy of Sciences, Lanzhou 730000, China; School of Physical Science and Technology, Lanzhou University, Lanzhou 730000, China; (3)School of Physical Science and Technology, Lanzhou University, Lanzhou 730000, China
  • 收稿日期:2006-09-22 修回日期:2006-10-20 出版日期:2007-07-20 发布日期:2007-07-04
  • 基金资助:
    Project supported by the National Natural Science Foundation of China (Grant Nos 10575119 and 10235030), the Knowledge Innovation Project (Grant No KJCX2-SW-N02) of Chinese Academy of Sciences, the Major State Basic Research Development Program of China (

Hyperon--hyperon interaction in relativistic mean field model

Li Ang(李昂)a)b)†, Zuo Wei(左维)a)b), Mi Ai-Jun(米爱军)b), and Burgio Gc)   

  1. a Institute of Modern Physics, Chinese Academy of Sciences, Lanzhou 730000, China; b School of Physical Science and Technology, Lanzhou University, Lanzhou 730000, China; c INFN Sezione di Catania, Via Santa Sofia 64, I- 95123 Catania, Italy 060853
  • Received:2006-09-22 Revised:2006-10-20 Online:2007-07-20 Published:2007-07-04
  • Supported by:
    Project supported by the National Natural Science Foundation of China (Grant Nos 10575119 and 10235030), the Knowledge Innovation Project (Grant No KJCX2-SW-N02) of Chinese Academy of Sciences, the Major State Basic Research Development Program of China (

PDF (PC)

623

赞

摘要： By using the new experimental data of \Lambda\Lambda potential, this paper has performed a full calculation for strange hadronic matter with different strangeness contents as well as its consequences on the global properties of neutron star matter in relativistic mean field model. It finds that the new weak hyperon--hyperon interaction makes the equations of state much stiffer than the result of the previous strong hyperon--hyperon interaction, and even stiffer than the result without consideration of hyperon--hyperon interaction. This new hyperon--hyperon interaction results in a maximum mass of 1.75M_{\odot} (where M_{\odot} stands for the mass of the Sun), about 0.2--0.5M_{\odot} larger than the previous prediction with the presence of hyperons. After examining carefully the onset densities of kaon condensation it finds that this new weak version of hyperon--hyperon interaction favours the occurrence of kaons in comparison with the strong one.

关键词: hyperon--hyperon interaction, equations of state, neutron star, kaon condensation

Abstract: By using the new experimental data of $\Lambda\Lambda$ potential, this paper has performed a full calculation for strange hadronic matter with different strangeness contents as well as its consequences on the global properties of neutron star matter in relativistic mean field model. It finds that the new weak hyperon--hyperon interaction makes the equations of state much stiffer than the result of the previous strong hyperon--hyperon interaction, and even stiffer than the result without consideration of hyperon--hyperon interaction. This new hyperon--hyperon interaction results in a maximum mass of 1.75M$_{\odot} $(where M$_{\odot}$ stands for the mass of the Sun), about 0.2--0.5M$_{\odot}$ larger than the previous prediction with the presence of hyperons. After examining carefully the onset densities of kaon condensation it finds that this new weak version of hyperon--hyperon interaction favours the occurrence of kaons in comparison with the strong one.

Key words: hyperon--hyperon interaction, equations of state, neutron star, kaon condensation

中图分类号:  (Nuclear matter)

  • 21.65.-f
21.30.-x (Nuclear forces) 21.60.-n (Nuclear structure models and methods) 26.60.-c (Nuclear matter aspects of neutron stars) 97.60.Jd (Neutron stars)