1974年9月10日白光耀斑研究  

STUDY OF THE WHITE LIGHT FLARE OF SEPTEMBER 10,1974

作　　者：胡菊[1] 方成[1] 丁明德[1] 

机构地区：[1]南京大学天文系

出　　处：《天文学报》1994年第4期396-405,共10页Acta Astronomica Sinica

基　　金：国家科委攀登计划资助;国家自然科学基金;教委博士点基金

摘　　要：本文详细分析了１９７４年９月１０日白光耀斑的光谱资料，并利用Ｎｏｎ－ＬＴＥ理论计算了它的半经验大气模型和辐射损失。由光谱测量得到：（１）连续辐射强度在巴耳末系限（３６４７）附近发生跳跃。在极大时刻，巴耳末跳跃可达约１１％；（２）该耀斑有强而宽的巴耳末谱线发射，其高项巴耳末谱线轮廓的全半宽随主量子数ｎ而变化，在８＜ｎ＜９达到极小；（３）连续辐射极大时刻同微波爆发极大相一致，比Ｈａ耀斑极大时刻提前几分钟。这三个特征很可能是Ⅰ类白光耀斑的典型特征。The spectra of the white light flare(WLF) of September 10,1974 have been analysed in detail.By use of Non-LTE theory,the semi-empirical model and the radiative losses of the WLF have been calculated.The spectral measurement indicated:(1)There was a Balmer jump near the Balmer limit(λ3647).At the maximum time,the jump attained about 11%; (2) The Balmer lines were strong and broad.The full-half widths of the line profiles varied with series number n and attained a minimum around 8<n<9;(3)The maximum time of the continuum emission coincided with the peak time of the microwave burst, but earlier by several minutes than the maximum time of Ha flare.These three characteristics are probably the typical properties for Type I WLFs.The analysis shows that the heating of the photosphere and the lower chromosphere of this WLF may be caused by the backwarming of the enhanced emissions from the upper chromosphere, while the heating of the upper chromosphere is probably due to the bombardment of high-energy electron beam.

关 键 词：太阳光谱 白光耀斑 半经验大气模型 

分 类 号：P182.52[天文地球—天文学]