一个新的太阳宇宙线的日-地传输模型

提出了一个新的太阳宇宙线日 -地传输的数学模型 ,它包括日冕粒子分布源和行星际传播方程 .根据对太阳宇宙线耀斑黑子群特征和耀斑相的观测 ,提出了多极性黑子湮没的两阶段日冕传输过程和传输方程 ,得到了与观测特征一致的日冕粒子分布源 .日冕传输的第一阶段 ,和太阳耀斑脉冲相的时间相当 ,加速粒子通过扩散很快均匀地分布在耀斑区 ,形成所谓快传播区 .第二阶段 ,加速粒子向快传播区以外的日冕区扩散并向行星际空间逃逸 ,形成慢传播过程 .日冕传输模型的数值结果和日冕传输的观测特征符合 .太阳宇宙线的行星际传播采用三维正交均匀各向异性方程描述 .最后把模型的数值结果与 1 997年 9月 2 4日事件的SOHO（SolarandHeliosphericObservatory）观测资料作了比较 .能较好地符合 .

A NEW MODEL FOR SOLAR-TERRESTRIAL PROPAGATION OF SOLAR COSMIC RAYS

A new solar terrestrial propagation model is presented for solar cosmic rays, which includes a coronal distribution source of flare particles and the propagation equation for solar cosmic rays in the interplanetary space. Based on observations of sunspot group characteristics of a solar cosmic ray flare and flare phases, a two step coronal transport model is proposed for solar flare particles, which results from the annihilations of sunspots in a sunspot group with magnetic multi polarities For the first step process, about as same period as impulsive phase, we obtain from the coronal transport model that the flaring region is filled uniformly with accelerated particles, it leads to the formation of Fast Propagation Region (FPR). During the second step process, after the flash phase, accelerated particles diffuse from the FPR into solar corona outside of the FPR and escape towards the interplanetary space, which is called the Slower Propagation Process. The interplanetary propagation of solar cosmic rays is described by the equation for solar cosmic ray propagation in an infinite, homogeneous and orthotropic medium. The intensity time profiles given by numerical calculations of the theory are compared with the observations for the event on 24 September 1997 from SOHO. The predicted results give a good fit to the data.