耀斑

Using series of vector magnetograms and proper motions, we have analyzed a delta spot in NOAA 9077. This delta spot formed and disintegrated in a very special way. Its current helicity evolution has a close relationship to the magnetic configuration. We find the conclusion, for the first time, that the sign reversal of the helicity can lead to the disintegration of the compact delta structure.

为了解NOAA 9077在7月14日的三维磁场位形，我们使用无力场局部外推程序模拟它的耀斑后环，探讨了理论与实际观测的差异和可能的原因；利用源表面方法，使用MDI高精度磁场数据进行全球势场外推，探讨2000年7月14日大耀斑事件的外部触发机制。

Hα line asymmetry is an important characteristics in spectral observations of chromospheric flare, since it reflects directly the dynamic process of solar flare.

Hα谱线轮廓的不对称性是色球耀斑光谱观测中的重要特征，也是耀斑动力学过程的重要观测事实之一。

Sol line asymmetry is an important characteristics in spectral observations of chromospheric flare, since it reflects directly the dynamic process of solar flare.

Hα谱线轮廓的不对称性是色球耀斑光谱观测中的重要特征，也是耀斑动力学过程的重要观测事实之一。

On the other hand, through the discussion on coronal density of flares, we found that the column mass density at the top of chromospheric flare model can not be represented the total mass above the chromosphere and the coronal density can be estimated from presure balance based on semiempirical model. Through estimations, the results show that the total mass above the chromosphere is about the same as the mass between the top of chromosphere and electron source, which so give an evidence that the source of electrons is situated at the top of flare loop.

另一方面，通过对日冕物质密度的讨论发现，半经验模型中色球顶部柱数密度不能用来代表耀斑环在日冕内的总物质，日冕物质密度可用日冕气压与半经验模型中色球顶部压力近似相等来进行估计，进而发现耀斑环在日冕内的总物质与前面估计的色球顶部到非热电子源之间的总物质近似相等，结果趋向于支持非热电子源位于环的顶部。

By comparison between SMM HXRBS observation and ground observation of Hα and CaIIK lines, especially through the combined study between SMM HXRBS observation and chromospheric flare models, the results show that: in the initial stage of impulsive phase, there is a correlative relation betweem Hα line intensity and hard X-ray emission; different spike in hard X-ray flux curve represents the burst at different location; the energy taken by non-thermal electron beam is larger than the radiative loss in chromosphere; for the flare studied here, the chromospheric evapporation is explosive; if the chromosphere is in balance between electron beam bombardment and radiative loss, the column mass density at the top of chromospheric flare model can not be taken as measure from the source of electrons and then the total material between the source of electrons and the top of chromosphere can be estimated.

通过一个具体耀斑的SMM HXRBS观测结果与同时基于地面得到的Hα和CaⅡK可见光谱观测结果对比，特别是将硬x谱观测结果与色球半经验模型联立研究，结果显示出：在脉冲相上升段，硬x发射与Hα辐射之间存在对应关系；硬x线光变曲线中不同脉冲爆发分量不太可能起源于同一位置；硬x辐射所反映的高能非热电子总携带能量大于色球总辐射损失；对所研究的耀斑而言，其色球蒸发过程是爆发性的；在详细比较了非热电子色球总沉积和色球辐射损失的基础上，指出半经验模型中色球顶部柱数密度不能看成是从非热电子源度量的，从而估计了色球顶部到非热电子源之间的总物质。

Lately static modelling have gradually replaced by hydrodynamical modelling.

近来耀斑静力学理论模型已逐步被耀斑动力学理论模型所取代。

However, these events were outshone by a flare on November 4 , 2003 that was the most powerful X-ray flare ever recorded.

然而，这些事件失色的耀斑11月4日， 2003年，是最强大的X射线耀斑以往任何时候都记录在案。

Based on a qualitative analysis of the data of the type IV radio burst and accompanying phenomena (post flare loops, radio pulsation in the decaying phase,multi-band emissions and mass ejection etc.)associated with the white light flare of 1991 June 6, it isproposed that the WLF and radio burst come from the sameelectron accelerating area in the low corona.

通过1991年6月6日共生太阳白光耀斑的射电运动IV型爆发及其伴随现象(包括耀斑后环、爆发衰减相的射电脉动、多波段射电辐射和太阳物质抛射等)观测资料的分析，定性地探讨了WLF的起源、加热机制和发射地点的问题。

The applications of the theory in robot translation parameter computation and in Qualitative Scene Model construction are presented.(3) Intrinsic Images and color constancy of Real Color Images Based on the Dichromatic Reflection Model proposed by Klinker [55] , it is the NO. 1 for this paper to measure the spectral relationship of a CCD color camera, to reestablish the linear relationship, to separate the illuminant and object color components in real color images, and to extract the intrinsic image and highlight image from the real color image, as well as to eliminate the influences of highlights upon the usual image segmentation algorithm.

以Klinker[55]等提出的&双色反射模型&为基础，首次测定了彩色摄像机的光强----灰度响应关系，恢复了摄像机的整体线性关系；首次在真实彩色图像（即由彩色摄像机直接获取的图像）中成功地分离了光照和景物的颜色；成功地抽取了本色图像和耀斑图像；在此基础上，又将双色反射模型成功地运用到真实彩色图像的分割方面，消除了耀斑对分割的影响。

Using the time-match semiempirical models for two flares (one is classified as a SB flare and the other a 2B flare), which were deduced from the spectral data obtained with the solar tower telescope of Nanjing University, we calculate the radiative loss at different phase of the flares.

针对我们已经建立的二个定态色球耀斑半经验模型，计算了耀斑不同时刻下的色球辐射损失速率，包括氢在四个能级假设下的所有跃迁、CaⅡ在五个能级下的所有跃迁、MgⅡ在三个能级下的所有跃迁、以及负氢离子的自由——自由和束缚——自由跃迁等。

I am sure after a few weeks of adaptation and familiarization I will have no difficulty in functioning on a daily basis in an English speaking society or in participating fully in graduate studies.

在大学的三年的学习生活不仅给予我自身的充实，更重要的是磨练和培养了我较强的自觉能力和严谨，踏实的作风以及不怕困难的精神，对未来充满了信心！

As the first volcanoes erupted, one of the gases that bellowed out was steam.

在第一批火山喷发时，喷出的气体之一就是水蒸汽。