coronal equilibrium

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。