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 ident...
【英文摘要】
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 ident...
【基金】
Supported by National Natural Science Foundation of China (10275029, 10675024)
【更新日期】
2009-08-26
【分类号】
O571
【正文快照】
A protoneutron star is now believed to be born as a result of the gravitational collapse of a massive evolved progenitor star (M ～ 8?25 M ) in Type-II supernova[1, 2]. Neutrinos of this star are prevented by their short mean free paths from running away
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