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, ∑, and (三) 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.
参考文献
| [1] | Bethe H A .[J].Reviews of Modern Physics,1990,62:801. |
| [2] | Burrows A;Hayes J;Fryxell B A .[J].Astrophysical Journal Letters,1995,450:830. |
| [3] | Burrows T J;Mazurck A;Lattimer J M .[J].Astrophysical Journal Letters,1981,251:325. |
| [4] | Burrows A;Lattimer J M .[J].Astrophysical Journal Letters,1986,307:178. |
| [5] | Keil W;Janka H Th .[J].Astronomy and Astrophysics,1995,296:145. |
| [6] | Tsuruta S;Cameron A G W .[J].Canadian Journal of Physics,1966,44:1863. |
| [7] | Schaab C;Weber F;Weigel M K et al.[J].Nuclear Physics A,1996,605:531. |
| [8] | Glendenning N K.Compact Stars[M].New York:springer-verlag,1997 |
| [9] | Boguta J;Bodmer A R .[J].Nuclear Physics A,1977,292:413. |
| [10] | Glendenning N K .[J].Astrophysical Journal Letters,1985,293:470. |
| [11] | Knorren R;Prakash M;Ellis P J .[J].Physical Review C,1995,52:3470. |
| [12] | Oppenheimer J R;Volkoff G .[J].Physical Review,1939,55:374. |
| [13] | Madappa Prakash;Ignazio Bombaci;Manju Prakash .[J].Physics Reports,1997,280:1. |
上一张
下一张
上一张
下一张
计量
- 下载量()
- 访问量()
文章评分
- 您的评分：
-
10%
-
20%
-
30%
-
40%
-
50%