By comparison of measured spatially resolved aluminum line radiation with calculated ones with coronal equilibrium, spatially resolved electron temperature of aluminum plane target was obtained.
35μm,70J,700ps)上,采用空间分辨晶体谱仪从发泡铝平面靶切向方向观测,测得了铝平面靶沿激光轴向方向发射的空间分辨线谱,理论上采用日冕模型计算,二者配合给出了铝靶电子温度空间分布0。
The solar total eclipse provides a good opportunity to observe the solar corona and is of significance for the researching of the corona [1,2] .
在１９９７ 年３ 月９ 日日全食时， 我们于黑龙江省漠河市（ 西林吉） 作了一系列日冕的照相观测不同感光的日冕像上显示出赤道东西的宽冕流、两极区冕洞、极羽和２０ 多条极射线等结构特征本文综合一些日冕像的形态结构和亮度测量结果，给出日冕的形态结构图、等亮度图、两极区和赤道区东西的亮度分布
more and more observational data about coronal loops have been obtained.
日冕加热是太阳物理中一个基本问题。
Using some data observed with SXT/HXT aboard Yohkoh and the Nobeyama Radioheliograph (NoRH) on 1998 April 23, a comprehensive study on the soft X ray coronal mass ejection (CME) on solar SE limb shows there were two magnetic dipole sources(MDSs), one magnetic capacity belt (MCB) between MDSs, one neutral current sheet (NCS) and only a few activation sources (ASs).
使用Yohkoh卫星上的SXT/HXT和Nobeyama射电日像仪 (NoRH)观测资料 ,对1 998年 4月 2 3日发生在日面东南边缘上的软X射线日冕物质抛射 (CME)作了分析研究 ,结果表明 ,软X射线CME具有两个磁偶极源 (MDSs) 。
Alfven waves propagate to go to a top of coronal loop by the photoshere along both feet of arch magnetic line of force.
来自太阳光球层的Alfven波沿着日冕环的拱形磁感线两足向上传播，在冕环的顶部两反向传播的波相遇，强烈的不稳定性可能激发起等离子体湍动。
Generally,the solar high energy particles in the flares are believed to be accelerated in two stages:acceleration by abrupt release of magnetic energy in the first stage and coronal diffusive shock wave or stochastic acceleration in the second stage.
考虑日冕区加速中相对论性粒子的扩散激波加速，结果表明：（１）粒子随时间的分布，其主要特点是随时问增加，一定能量的粒子分布迅速增加至最大后下降，并且能量越大，其最大就越向着大时间移动；（２）给出了相应的时间积分谱，它正比于具有指数截止的粒子动量的幂律。