太阳宇宙线源物质的高色球层模式和重离子丰度过量机制的探讨

本文利用太阳能量粒子事件中重离子平均丰度过量的资料,计算得到太阳能量粒子源物质的温度,提出了描述太阳宇宙线能量粒子源物质的新模式——高色球层模式;太阳耀斑观测确定,太阳宇宙线耀斑的加速区一般最可能出现在低日冕甚至高达几万公里的高度,从而,太阳宇宙线的源和加速区通常不位于同一区域;进而提出了描述太阳能量粒子事件中重离子丰度过量的可能机制——其源物质是通过太阳黑子的冻结型无力场从高色球层输送到活动区,形成耀斑前加速区内重离子丰度大和耀斑后宇宙线中重元素丰度的过量. 

SOURCE MATERIAL OF SOLAR ENERGETIC PARTICLES FROM THE HIGH CHROMOSPHERE AND OVERA- BUNDANCE OF HEAVY IONS BY THE FORCE- FREE FIELD OF SUNSPOTS

This paper presents a new idea by modelling the high chromosphere of source material of solar energetic particles. Based on the temperature as determined by the data of overabundance of heavy ions relative to local galactic abundances in solar energetic particle events, the high chromosphere is suggested to be the source of solar energetic particles. According to a great number of observations, the acceleration region of solar energetic particles during solar flares is most likely to occur in the low corona and even up to tens thousand kilometres height. Therefore, the source region of solar cosmic rays is generally not so same as that of the particle acceleration. Moreover, the author presents further a model of mechanism of overabundance of heavy ions in solar energetic particle events. From the model, the heavy nuclei with low first-ionization potentials in the source are preferentially affected by electromagnetic force of force-free field in the frozen magnetic field of sunspot and are transported to sunspot region by this action, their abundances are larger in the acceleration region before the onset of solar flares and are overabundant in solar cosmic rays.