K . we still cannot completely explain why the temperature of the chromosphere and corona can be higher than the photosphere 度。为甚么日冕和色球层的温度可以比光球层更高，仍是天文学上一个未解之谜。
As one of the major problems in solar - terrestrial physics , coronal heating has kept to attract physicists " attention for a few decades 近半个多世纪以来，日冕加热问题一直都是日地物理学界关注研究的难题。
Invisible to optical devices , the halo can be seen by fuse as a blue , football - shaped envelope around the galaxy 光学仪器是看不见这种日冕的，通过fuse可看到，这种日冕围绕在银河系周围，象一个蓝色足球形状的外壳。
In this thesis , we investigate the role of alfven wave in the coronal heating process . all the work consists of two main parts 我们从两个方面对这个问题进行了探讨：第一个方面主要地研究了加热日冕的alfven波源。
Above and below the galactic plain , in which earth and our solar system reside , they detected an extremely thin , hot gas corona , or halo 在这上下居住着地球和我们的太阳系的星系平原上，科学家发现一种极薄的热气日冕。
Then , torsional alfven waves propagate upwards along the coronal loop and the carried wave energy can make a play in coronal heating 当被激发的扭转alfven波沿着磁通管向上传播到达日冕，其携带的能量就可以加热日冕。
So we conclude that observed electron energy spectrum about 10 mev in large flare may be produced by the acceleration of synchrotron radiation 因此我们认为太阳耀斑中10mev左右的能谱是由同步加速辐射加速日冕快电子产生的。
The planet and its neighbours are bathed in the solar wind , a stream of charged particles ejected from the upper atmosphere of the sun 地球及其邻居都受到太阳风? ?一股从太阳最外层的大气（日冕）喷射出来的带电粒子流? ?的侵袭。
Zheng , h . n . , zhang , b . and wang , s . , 1995 , a mechanism for the formation of plasmoid - type cme in the solar corona , acta astron . sinica , 36 , 341 郑惠南，张兵，王水, 1995 ，等离子体团型日冕物质抛射的形成机制，天文学报， 36 , 341
Day mian side go up , even xie have made curious brilliance , radiate outward , arise especially big light beam , astronomer name is " mian flow " 日冕的边上，甚至泻出了奇异的光彩，向外辐射，出现特大的光束，天文学家称之为“冕流” 。
