摘要
本文简要回顾了耀斑中正负电子湮灭线的形成过程，着重研究了一个强γ射线耀斑０ ．５１１ ＭｅＶ 线随时间的演化。结果表明，为解释观测数据，加速质子谱必须随时间变化， 从而间接地提出了一种基于０ ．５１１ ＭｅＶ 线获取加速质子谱演化信息的新途径。
The origin of 0.511 MeV line in solar flares is briefly reviewed. Taken the flare of 16 December 1988 as an example, we studied the time profile of the 0.511 MeV line flux. It is found that in order to match the observations, the spectrum of injected energetic particles should be varied during the flare. The justness of deducing the spectral evolution based on 0.511 MeV line time profile is therefore discussed.
