查询词典 flare-out

The HeⅠ 10830 profiles of the flare are relatively broad and can not be simulated by Doppler broadening mechanism with a uniform flare model atmosphere.

该耀斑的HeⅠ 10830谱线线翼相对较宽，不能用均匀耀斑模型的纯Doppler加宽机制解释。

Flare-Tip The flare-tip is typically a "shaft-over" hosel, meaning the shaft covers the top of the hosel where the two connect.

Flare-Tip：该特点在於杆颈插在杆身内，也就是说杆颈的最上端是在杆身末端内。

Some people introduce subphotosphere magnetic charges or dipole, which can fit magnetic field on the photosphere, then the separatrix and separator above and on the photosphere can be located, the comparison between their location and location of flare ribbon support the idea of magnetic reconnection. It is called Source Method. Some people extrapolate magnetic fields of photosphere to corona by some method, then use QSLs method to investigate the relations between flare ribbons and magnetic field topology. Some people study relations between flare ribbons and singular point on the plane above photosphere. Some people investigate magnetic topology by analyzing magnetic field of photosphere directly.

或者以观测的光球磁场为基础，来构造光球下的磁荷或磁偶极等光球下磁源，进而研究光球上的磁拓扑结构与耀斑的关系；或者利用各种外推方法将光球磁场进行外推，然后用准分隔层的方法来研究磁拓扑结构与耀斑的关系；或者利用势场模型外推光球磁场，然后研究光球之上平行于光球的某一平面的两维奇点与耀斑的关系；或者直接利用观测的光球矢量场来研究磁场拓扑。

Eight models were constructed and divided into two groups by different cement thickness. In each group, there were two stems with high and low flare that implanted in both normal and stovepipe canal models respectively.

本研究藉由8 种模型以同骨水厚分为2 组，2 组分别将low flare 与high flare 骨柄分别植入正常与烟囱型股骨髓腔。

Results No patients in absorbent bandage group occurred skin injury, skin sensitiveness, itch, flare and blister, while 25 patients in coated fabric group occurred cadmia sensitiveness, skin flare, itch and several blisters whic h needed to be treated with medicine.

结果脱脂绷带打结牵引组患者无1例出现皮肤损伤和皮肤过敏、发痒、红肿、水疱等症状。胶布粘贴牵引组有25例患者出现氧化锌过敏，皮肤发红发痒，并有多个小水疱，需敷药治疗。

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。

Five papers are included in the part, which entitled as semiempirical models of the impulsive phase of the chromospheric flare, a study of the energy deposits in flaring atmosphere with semiempirical models of flares, spectral line asymmetry of solar flare, combined study between SMM HXRBS observation and semiempirical models, and continuum emission of white-light flare.

论文的上篇由5篇文章组成，形成了研究耀斑半经验模型的一个系列，其内容除了构造半经验模型外，着重在半经验模型基础上作扩展性研究，包括探讨耀斑的能量过程，计算谱线轮廓的不对称性，讨论白光耀斑连续发射的大气特征，以及寻求高能观测结果与半经验模型的联系等。

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。

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。