The competition of neutrino energy loss due to the pair, photo-, plasma process at the late stages of stellar evolution

LIU Jing-Jing

doi:10.1088/1674-1137/33/1/004

Chinese Physics C> 2009, Vol. 33> Issue(1) : 15-19 DOI: 10.1088/1674-1137/33/1/004

The competition of neutrino energy loss due to the pair, photo-, plasma process at the late stages of stellar evolution

LIU Jing-Jing ^,

The Department of Physics, Qiongzhou University, Wuzhishan 572200, China

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Abstract：
Based on the Weinberg-Salam theory, the competition of the Neutrino Energy Loss (NEL) rates due to the pair, photo- and plasma process are canvassed. The ratio factor C₁, C₂ and C₃ which correspond the different contributions of the pair, photo- and plasma neutrino process to those of the total NEL rates are accurately taken into account. The ratio factors are very sensitive to the temperature and density. The ratio factor C₂ always is lower than the ratio factor C₁ and C₃. The pair NEL process is the dominant contribution before the
crossed point O(C₁ =C₃=0.45) and the plasma NEL process will be the main dominant contribution after the crossed point O. With increasing temperature, the crossed point $O$ will move to the direction of higher density.

References

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LIU Jing-Jing. The competition of neutrino energy loss due to the pair, photo-, plasma process at the late stages of stellar evolution[J]. Chinese Physics C, 2009, 33(1): 15-19. doi: 10.1088/1674-1137/33/1/004

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Received: 2007-12-12
Revised: 2008-06-16

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沈阳化工大学材料科学与工程学院沈阳 110142

The competition of neutrino energy loss due to the pair, photo-, plasma process at the late stages of stellar evolution

Corresponding author: LIU Jing-Jing,

The Department of Physics, Qiongzhou University, Wuzhishan 572200, China

Received Date: 2007-12-12

Accepted Date: 2008-06-16

Available Online: 2009-01-11

Abstract:

Based on the Weinberg-Salam theory, the competition of the Neutrino Energy Loss (NEL) rates due to the pair, photo- and plasma process are canvassed. The ratio factor C₁, C₂ and C₃ which correspond the different contributions of the pair, photo- and plasma neutrino process to those of the total NEL rates are accurately taken into account. The ratio factors are very sensitive to the temperature and density. The ratio factor C₂ always is lower than the ratio factor C₁ and C₃. The pair NEL process is the dominant contribution before the
crossed point O(C₁ =C₃=0.45) and the plasma NEL process will be the main dominant contribution after the crossed point O. With increasing temperature, the crossed point $O$ will move to the direction of higher density.

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The competition of neutrino energy loss due to the pair, photo-, plasma process at the late stages of stellar evolution

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