查询词典 flare

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。

Under a fixed model of chromospheric flare, we investigate the influences of Hα and CaIIK line profilles on various velocity distributions from semiempirical view. The results show that: Hα line is very sensitive to the velocity in upper chromosphere; the profile of CaIIK line have responses to velocity in any layer of chromosphere, but the degree of CaIIK line asymmetry is much weaker than that of Hα and can be ignored if velocity is as small as 10km/s; chromospheric condensation in lower part of transition region have strong influence on Hα line but contrary to CaIIK line, the typical characteristic of H line effected by chromospheric condensation in transition region is reversed blue asymmetry, i.e. the intensity of blue peak is stronger than that of red peak; the stronger the chromosphoric condensation is, the more obvious the Hα line asymmetry appears; and so on.

在确定的大气模型下，从半经验角度系统地研究了大气各个层次的速度场和运动结构对Hα和CaⅡK谱线轮廓的影响，得到；Hα线对色球上部速度场敏感，而对色球下部和温度极小区附近速度场不敏感；CaⅡK对整个色球速度场均有反应，但不对称性较Hα弱，且速度小于10km/s时不对称性很不明显；CaⅡK受过渡区色球凝聚的影响较弱，而Hα对色球凝聚十分敏感；色球凝聚影响Hα轮廓的典型特征是呈反转结构的兰不对称性，即兰峰强于红峰；色球凝聚越强，Hα不对称性也越显著：等。

The main characteristics include: the quiet Sun corona has a rapid response to the flare heating, within 2 second the corona temperature increases nearly one order of magnitude, but later such increase becomes very slowly; the downward velocity at early stage of impulsive phase is too small to be negnected; chromospheric evaporation made by conduction shows some intensely, the maximum evaporated velocity may be as large as 1000 km/s; the chromospheric condensation appears just when the chromospheric evaporation takes place and its place always coincide with that of transition region in the early stage; the maximum of chromospheric condensation occurs also in the early stage of impulsive phase, at which the density in condensation may be larger two order of magnitude than that of surround and the downward velocity may be as large as 100 km/s; after the maximum of chromospheric condensation, its strongth decreases gradually but its width becomes greater with time and have a tendency to transport into deep chromosphere; the front of chromospheric condensation heats atmosphere obviously and the temperature in the chromospheric condensation is higher than the original case; the downware velocity of transition region may be greater than 100 km/s at the early stage; when the evaporated material collide at the top of loop, the densityand the presure there increase rapidly, which result in the formation of a shock wave; and so on.

在改善色球辐射损失和精确分辨过渡区的基础上，通过联立求解连续性方程、动量方程和能量方程，构造了一维磁限制性耀斑环在热沉积作用下的大气动力学模型，获得了耀斑热模型下脉冲相早期较为细致的大气演化理论图象，其主要特征是：耀斑对宁静日冕的加热相当迅速，仅2秒钟日冕温度增加即达一个量级，之后日冕温度增加缓慢；脉冲相早期日冕向下速度很小，几乎可以忽略，热传导驱动色球蒸发，其过程较为激烈，蒸发极大速度可达到1000km/s；色球压缩区与色球蒸发几乎同时形成，且在早期其位置总是与过渡区位置重合；色球压缩极大发生在脉冲相早期，其时密度可高于周围约2个量级，向下速度可超过100km/s；色球压缩极大后，其强度逐渐减弱，但宽度明显增大，且渐渐脱离过渡区往色球传播；压缩区内物质温度要高于原先的大气温度；过渡区下降在脉冲相早期相当迅速，可超过100km/s；当蒸发物质在环顶高速相碰时，环顶的密度、压力迅速增大，且温度也有所增加，导致形成激波，其波面以每秒上百公里的速度自环顶向下传播；在脉冲相前期，日冕软x辐射对色球的加热作用可以忽略；等。

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。

This is why Yang Yong's work always radiates a certain flare of cinematographic charm.

这就是为何杨勇的作品总是散发出一种特殊的电影摄影般的闪耀魅力。

The coking performance of flare gas and it's kinetic were studied.

研究了火炬气结焦的性能及其动力学。

The second part pays attentions to the hydrodynamical model of solar flare (chromosphere+corona).

论文的下篇则致力于建立耀斑大气动力学理论模型，包括现有耀斑动力学模型评述，构造动力学模型的理论框架，耀斑主相动力学模型，以及耀斑脉冲相动力学模型等四章。

For raising the accuracy of the diagnasis ancl treatinemt of ALH We realised of 86 patients with diagnosis of Autoimmune liver disease, strictly defined by the criteria for diagnosis of autoimmune hepatitis or the results of liver histology, and tested its biochemical, serological, histological results. AIH patients were main women female 75 cases, male 11 cases, main in 40 - 60 years old ,AIH characterized by a flare of ALT, AST, elevated immunoglobulin G,γ-immunoglobulin: ALP, IgG, and presence of antinuclear antibody (81.5%); moderate or severe periportal or periseptal lymphocytic piecemeal necrosis.

为提高对自身免疫性肝炎的诊治水平，采用国际自身免疫性肝炎小组新修订的描述性诊断标准和计分系统，对符合诊断的患者进行临床、生化、病理特点分析。86例AIH患者，女75例，男11例，高发年龄为40～60岁，其中Ⅰ型80例(93.020k)，Ⅱ型3例(3.49％)；Ⅲ型3例(3.49％)；肝功能生化检查表现为肝炎样改变；实验室检查主要表现为高γ球蛋白血症，高IgG、ALP、γ-GT及甘油三酯增高，81.5％患者抗核抗体阳性：病理改变以界板性肝炎，浆细胞浸润为主，78％的患者对免疫抑制剂治疗效佳。

The split between the two groups can hardly be papered over.

这两个团体间的分歧难以掩饰。

This approach not only encourages a greater number of responses, but minimizes the likelihood of stale groupthink.

这种做法不仅鼓励了更多的反应，而且减少跟风的可能性。