Pair neutrino energy loss for nuclei ^(56)Fe at the late stages of stellar evolution  

作　　者：刘晶晶 罗志全 

机构地区：[1]Institutes of Theoretical Physics, China West Normal University, Nanchong

出　　处：《Chinese Physics C》2008年第8期617-619,共3页中国物理C（英文版）

基　　金：National Natural Science Foundation of China (10347008);Scientific Research and Fund of Sichuan ProvincialEducation Department (2006A079)

摘　　要：t Based on the Weinberg-Salam theory, the pair neutrino energy loss rates for nuclei 56^Fe are canvassed for the wide range of density and temperature. The results of ours （QLJ） are compared with those ofBeaudet G, Petrosian V and Salpeter E. E＇s （QBPs）, and it shows that the pair neutrino energy loss rates of QBPS are always larger than QLJ .The QBPS is 12.57%, 12.86%, 14.99%, 19.80% times higher than QLJ corresponding to the temperature T9=0.385, 1.0, 5.0, 10, respectively.t Based on the Weinberg-Salam theory, the pair neutrino energy loss rates for nuclei 56^Fe are canvassed for the wide range of density and temperature. The results of ours （QLJ） are compared with those ofBeaudet G, Petrosian V and Salpeter E. E＇s （QBPs）, and it shows that the pair neutrino energy loss rates of QBPS are always larger than QLJ .The QBPS is 12.57%, 12.86%, 14.99%, 19.80% times higher than QLJ corresponding to the temperature T9=0.385, 1.0, 5.0, 10, respectively.

关 键 词：Weinberg-Salam theory pair neutrino energy loss stellar evolution 

分 类 号：O571[理学—粒子物理与原子核物理]