耀斑

The first part deals mainly with the chromospheric flare from the semiempirical view.

本论文的研究正是涉及耀斑大气研究的这两个主要方面。

Comparing the SXR and microwave data with the optical data leads to the following scenario: the corona has been already heated to some extent before flare onset, and in the first two minutes of the impulsive phase, heat conduction was the main source or, at least, a competitive source, for chromospheric heating.

把软X射线和微波资料与光学资料比较研究，我们得到如下图象：在耀斑触发前，日冕已经加热到一定程度；在脉冲相的前两分钟里，热传导是色球加热的主要的或至少是极富竞争力的机制。

Summarizing the results above, we further obtained: Hα blue asymmetry observed usually in the early stage of flares may be caused by chromospheric condensation in transition region; the Hα red asymmetry appeared later may be resulted from the downward movement of upper chromosphere; and still later CaIIK asymmetry may be explained to have 10-20 km/s downward velocity in middle or lower part of chromosphere, This explanation is self-consistent among the observations of Hα and CaIIK line during the flare.

综合所有计算的不对称特征，我们进一步得到：耀斑早期的短时间兰不对称性可由过渡区里的色球凝聚引起，随后的红不对称性是色球上部物质向下运动的结果，而后来出现的CaⅡK不对称特征则表明色球中下部具有10-20km/s的向下运动速度。

The data such as the Hα-spectrum-spectroheliographic observations, the Hα-chromospheric observations, etc., of a flare loop prominence which occurred on the western solar limb on 1981 April 27 have been obtained at Yunnan Observatory, Academia Sinica.

云南天文台摄取1981年4月27日太阳西边缘的一个耀斑环珥的H_α光谱太阳分光照像(S~2HG)和H_α色球照像等资料。

So in the field of solar flare atmosphere, semiempirical modelling and hydrodynamical modelling of solar flare are main contents.

因此，目前在耀斑大气研究方面，半经验模型和动力学理论模型是主要内容。

One is semiempirical modelling, the other is theoretical modelling. The former have developed recently from the average model into the time-match model. The latter includes further static modelling and hydrodynamical modelling.

半经验模型的研究近来已从平均模型逐步发展到定态模型，即针对具体的耀斑就不同时刻下所获得的光谱资料建立不同时刻下的大气模型，以研究大气结构随时间的变化。

It is studied for the detailed morphological and dynamic evolution of several disturbed filaments, the relevant changes of photospheric magnetic field and coronal structure, as well as the development of associated flares.

我们详细研究了几个扰动暗条的位形和动力学演化、相关的光球磁场和日冕结构的变化，以及相联系的耀斑发展。

Pixilated . Low-light filming is grainy, and any bright image source tends to flare badly, but is on the whole acceptable.

低光拍摄是呈粒状，和任何美好的形象的来源往往耀斑严重，但就整体而言是可以接受的。

The preliminary and promising theory of 3D magnetic reconnection can lead us to the real understanding of solar flares.

三维磁重联的提出极大的提高了人们对太阳耀斑本质的认识。

The soft X-ray flux of X class flares increases the ionisation of the upper atmosphere, which can interfere with short-wave radio communication, and can increase the drag on low orbiting satellites, leading to orbital decay.

在软X射线磁通的X级耀斑增加了离子化的高层大气，从而干扰短波无线电通讯，并可以增加拖累低轨道卫星，从而导致轨道衰减。

According to the clear water experiment, aeration performance of the new equipment is good with high total oxygen transfer coefficient and oxygen utilization ratio.

曝气设备的动力效率在叶轮转速为120rpm～150rpm时取得最大值，此时氧利用率和充氧能力也具有较高值。

The environmental stability of that world - including its crushing pressures and icy darkness - means that some of its most famous inhabitants have survived for eons as evolutionary throwbacks, their bodies undergoing little change.

稳定的海底环境─包括能把人压扁的压力和冰冷的黑暗─意谓海底某些最知名的栖居生物已以演化返祖的样态活了万世，形体几无变化。