Optical observations of the solar corona at total solar eclipse
日全食时的日冕光学观测
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。
intermediate corona
中介日冕-中等太阳活动时的日冕
Fraunhofer component
日冕光谱夫琅和费部分
quiet coronal X-ray emissio
宁静日冕Ｘ射线辐射
In this paper the author expound mainly the current status in the research of solar quiet corona, coronal holes and heating mechanism of corona.
主要论述宁静日冕和冕洞，以及日冕加热问题的研究现状。
coronograph and similar instruments, for observing the sun's corona
日冕仪和用于观察太阳日冕的类似仪器
POLARIZATION OBSERVATION OF THE SOLAR CORONA AT THE SOLAR ECLIPSE OF 1968 SEPTEMBER 22.
1968年9月22日日食的日冕偏振观测
On the other hand, all the material in the transversal sheet comes from the corona and produces a high-temperature coronal loop.
横向电流片的物质则全部来自日冕,从而形成高温日冕环。
Polarization Observation of White Light Corona during the Total Solar Eclipse on 2006 March 29
2006年3月29日日全食白光日冕偏振测量(英文)
Coronal structure and brightness profile of the total solar eclipse on August 1,2008
2008年8月1日日全食的日冕结构和亮度分布
non-Fraunhofer component
非夫琅和费部分-日冕光谱
The corona gains and loses energy continuously.
日冕总是不断地获得能量和损失能量。
The continuum of the corona is essentially radially polarized.
日冕连续区基本上是经向偏振。
Computing the Coronal Temperature by Using the Filter Ratio Method;
用Filter Ratio方法计算太阳日冕温度
THE GREEN CORONAL LINE ABOVE ACTIVE REGION AT SOLAR LIMB ON 5 AUG. OF 1989
1989年8月5日太阳边缘活动区之上的绿日冕线
One other interesting aspect of the relation of coronal holes to the solar wind follows from the appearance of coronal holes at the poles.
日冕洞与太阳风的关系的另一个有趣的方面是日冕洞在两极的形状。
From the significance of the observation and research of the solar corona, the necessity of setting up the observation of the solar corona at the Yunnan Observatory is explained in this present article.
本文从日冕观测和研究的意义出发,说明云南天文台建立日冕观测的必要性。
We show that both the preevent corona and the driving mechanism are important in the formation and evolution of CMEs.
结果表明,初态日冕和驱动机制对日冕物质抛射的形成及演化都有重要影响.
Looking at small details we find that the corona has a delicate structure.
仔细研究细节后，我们发现日冕有精细结构。