Thermal protoneutron stars with hyperons  

作　　者：喻孜 刘广洲 朱明枫 丁文波 赵恩广 

机构地区：[1]Physics Department of Jilin University [2]Institute of Theoretical Physics, Chinese Academy of Science

出　　处：《Chinese Physics C》2009年第S1期70-72,共3页中国物理C（英文版）

基　　金：Supported by National Natural Science Foundation of China (10275029, 10675024)

摘　　要：The properties of thermal protoneutron star matter including hyperons are investigated in the framework of the relativistic mean field theory (RMFT). In protoneuron star matter, with the increase of the temperature, the critical densities of hyperons decrease, the sequence for appearances of hyperons change, the abundances of hyperons as well as neutrinos increase, and the strong interactions between baryons get weaker. Meanwhile, the abundances of isospin multiple states for nucleons, Σ, and ■ become identical, leading to isospin saturated symmetric matter, respectively. Moreover, if a protoneutron star is born with higher temperature, it is less likely to convert to a black hole.The properties of thermal protoneutron star matter including hyperons are investigated in the framework of the relativistic mean field theory (RMFT). In protoneuron star matter, with the increase of the temperature, the critical densities of hyperons decrease, the sequence for appearances of hyperons change, the abundances of hyperons as well as neutrinos increase, and the strong interactions between baryons get weaker. Meanwhile, the abundances of isospin multiple states for nucleons, Σ, and ■ become identical, leading to isospin saturated symmetric matter, respectively. Moreover, if a protoneutron star is born with higher temperature, it is less likely to convert to a black hole.

关 键 词：neutron star finite temperature HYPERONS 

分 类 号：O571[理学—粒子物理与原子核物理]