Cosmic-Ray Positrons Produced by Pulsar Winds from Mature Gamma-Ray Pulsars

查看全文 作　　者：[1,2,3]张力;[1,2]K.S.Cheng;[1,2,3]梅冬成 机构地区：[1]Department of Physics,Yunnan University,Kunming 650091;[2]Department of Physics,University of Hong Kong,Pokfulam Road,HongKong;[3]Yunnan Observatory,Chinese Academy of Sciences,Kunming 650011 出　　处：《Chinese Physics Letters》索引2001年第18卷第5期,共4页 基　　金：Supported by the Natural Science Foundation of Yunnan Province under Grant No.98A140R;an RGC grant of the Hong Kong Government;Subsidized by the Special Funds for Major State Basic Research Projects. 摘　　要：In the frame of theγ-ray pulsar outer gap model,e^(±)pairs in the pulsar magnetosphere are produced by the cascade of e^(±)pairs through synchrotron radiation of the return current from the outer gap.These pairs are accelerated mono-energetically to relativistic energies in the pulsar wind driven by low-frequency electromagnetic waves.Using Monte Carlo simulations,we generate a sample of the matureγ-ray pulsars in our Galaxy and calculate the positron production rate from these pulsars.With a simple leaky box model,we calculate the ratio of cosmic-ray positron to total electrons.Our result indicates that the pulsar contribution to the cosmic ray positron peaks at about 40 GeV and the observed e^(+)/(e^(-)+e^(+))ratio can be explained by this model. 关 键 词：COSMIC outer RETURN