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

[1]

. Gamow G, Schonberg M. Phys. Rev., 1941, 59: 5392. Fuller G M, Fowler W A, Newman M J. AP. J, 1980, 42:447; Fuller G M, Fowler W A, Newman M J. AP. J, 1982,252: 715; Fuller G M, Fowler W A, Newman M J. AP. J,1982, 48: 279; Fuller G M, Fowler W A, Newman M J. AP.J, 1985, 293: 13. LIU J J, LUO Z Q. Chinese Physics C (HEP NP), 2008,32: 1864. LIU J J, LUO Z Q, LIU H L, LAI X J. International Journal of Modern Physics A, 2007, 22: 33055. LIU J J , LUO Z Q. Chinese Physics Letter, 2007, 24: 18616. LIU J J , LUO Z Q. Chinese Physics, 2007, 16: 36247. Esposito S, Mangano G, Miele G, Picardi I, Pisanati O.Nuclear Physics B, 2003, 658: 2178. Indranath Bhattacharyya J. Phys. G, 2006, 32: 9259. Beaudet G, Petrosian V, Salpeter E E. AP. J, 1967, 150:97910. Dicus D A. Phys. Rev. D, 1972, 6: 94111. Munakata H, Kohyama Y, Naoki Itoh. AP. J, 1985, 296:19712. Itoh N, Adachi T, Nakagawa M, Kohyama Y, Munakata H.AP. J, 1989, 339: 35413. Itoh N, Mutoh H, Hikita A, Kohyama Y. AP. J, 1992, 395:62214. Itoh N, Hayashi H, Nishikawa A, Kohyama Y. AP. J, 1996,102: 41115. Weinberg S. Phys. Rev. Letter, 1967, 19: 126416. Salam A. Elementary Particle Physics. Ed. Svartholm N.1968. 36717. Kohyama Y, Itoh N, Munakata H. AP J, 1986, 310: 81018. Sirlin A. Phys. Rev. D, 1980, 22: 971

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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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