Thermal protoneutron stars with hyperons

YU Zi; LIU Guang-Zhou; ZHU Ming-Feng; DING Wen-Bo; ZHAO En-Guang

doi:10.1088/1674-1137/33/S1/023

Chinese Physics C> 2009, Vol. 33> Issue(S1) : 70-72 DOI: 10.1088/1674-1137/33/S1/023

Thermal protoneutron stars with hyperons

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Abstract：
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 Ξ 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.

References

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YU Zi, LIU Guang-Zhou, ZHU Ming-Feng, DING Wen-Bo and ZHAO En-Guang. Thermal protoneutron stars with hyperons[J]. Chinese Physics C, 2009, 33(S1): 70-72. doi: 10.1088/1674-1137/33/S1/023

YU Zi, LIU Guang-Zhou, ZHU Ming-Feng, DING Wen-Bo and ZHAO En-Guang. Thermal protoneutron stars with hyperons[J]. Chinese Physics C, 2009, 33(S1): 70-72. doi: 10.1088/1674-1137/33/S1/023 shu

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Received: 2008-10-22
Revised: 1900-01-01

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沈阳化工大学材料科学与工程学院沈阳 110142

Thermal protoneutron stars with hyperons

Corresponding author: LIU Guang-Zhou,

Received Date: 2008-10-22
Accepted Date: 1900-01-01
Available Online: 2009-01-10

Abstract: 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 Ξ 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.