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Chinese Physics C> 2009, Vol. 33> Issue(10) : 834-837 DOI: 10.1088/1674-1137/33/10/003

Plasma neutrino energy loss due to the axial-vector current at the late stages of stellar evolution

  •  (Department of Physics, Qiongzhou University, Wuzhishan 572200, China)

  • Based on the Weinberg-Salam theory, the plasma neutrino energy loss rates of vector and axial-vector contributions are studied. A ratable factor of the rates from the axial-vector current relative to those of the total neutrino energy loss rates is accurately calculated. The results show that the ratable factor will reach a maximum of 0.95 or even more at relatively higher temperature and lower density (such as ρμe<107 g/cm3). Thus the rates of the axial-vector contribution cannot be neglected. On the other hand, the rates of the axial-vector contribution are on the order of ~0.01% of the total vector contribution, which is in good agreement with Itoh's at relatively high density (such as ρμe>107 g/cm3) and a temperature of T≤1011K.

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    [1] . Hirata K et al. Phys. Rev. Lett., 1987, 58: 14902. Bionta R M et al. Phys. Rev. Lett., 1987, 58: 14943. Fuller G M, Fowler W A, Newman M J. Astrophys. J.,1980, 42: 447; Fuller G M, Fowler W A, Newman M J.Astrophys. J., 1982, 252: 7154. Esposito S, Mangano G, Miele G et al. Nucl. Phys. B., 2003,658: 2175. LIU J J, LUO Z Q. Chinese Physics C (HEP NP), 2008,32: 1866. LIU J J, LUO Z Q, LIU H L, LAI X J. International Journalof Modern Physics A, 2007, 22: 33057. LIU J J, LUO Z Q. Chinese Physics Letter, 2007, 24: 18618. LIU J J, LUO Z Q. Chinese Physics, 2007, 16: 36249. LIU J J. Chinese Physics C (HEP NP), 2009, 33: 1510. Adams J B, Ruderman M A, Woo C H. Phys. Rev., 1963,129: 138311. Dicus D A. Phys.Rev. D, 1972, 6: 94112. Kohyama Y, Itoh N, Munakata H. Astrophys. J., 1986, 310:81513. Itoh N, Mutoh H, Hikita A et al. Astrophys. J., 1992, 395:62214. Weinberg S. Phys. Rev. Letter, 1967, 19: 126415. Salam A. In Elementary Particle Physics ed N Svartholm(Stockholm, Almqvist and Wiksells) 1968, 36716. Sirlin A. Phys. Rev. D, 1980, 22: 97117. Beaudet G, Petrosian V, Salpeter E E. Astrophys. J., 1967,150: 979

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LIU Jing-Jing. Plasma neutrino energy loss due to the axial-vector current at the late stages of stellar evolution[J]. Chinese Physics C, 2009, 33(10): 834-837. doi: 10.1088/1674-1137/33/10/003
LIU Jing-Jing. Plasma neutrino energy loss due to the axial-vector current at the late stages of stellar evolution[J]. Chinese Physics C, 2009, 33(10): 834-837.  doi: 10.1088/1674-1137/33/10/003 shu
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Received: 2008-10-20
Revised: 2008-12-20
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Plasma neutrino energy loss due to the axial-vector current at the late stages of stellar evolution

    Corresponding author: LIU Jing-Jing,
  • (Department of Physics, Qiongzhou University, Wuzhishan 572200, China)
  • Received Date: 2008-10-20
  • Accepted Date: 2008-12-20
  • Available Online: 2009-10-05

Abstract: 

Based on the Weinberg-Salam theory, the plasma neutrino energy loss rates of vector and axial-vector contributions are studied. A ratable factor of the rates from the axial-vector current relative to those of the total neutrino energy loss rates is accurately calculated. The results show that the ratable factor will reach a maximum of 0.95 or even more at relatively higher temperature and lower density (such as ρμe<107 g/cm3). Thus the rates of the axial-vector contribution cannot be neglected. On the other hand, the rates of the axial-vector contribution are on the order of ~0.01% of the total vector contribution, which is in good agreement with Itoh's at relatively high density (such as ρμe>107 g/cm3) and a temperature of T≤1011K.

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