查询词典 chromospheric

Chromospheric Activity of Arcturus Observed at Call H and K Lines on February 14, 1984

1984年2月14日大角星色球活动的CaⅡ H，K线观测

It is known 19 that chromospheric activity correlates with stellar rotation.

我们知道恒星的自转速度和色球层的活动二者是相关的（参考文献19）。

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。

But meticulous analysis show chromospheric activity of evolution stars depend on stellar spectral type and effective temperature strongly.

通过主序星的色球活动对恒星色指数不同依赖关系的研究，我们分析了Vaughan—Preston间隙产生的原因，分析结果显示恒星的年龄在这一间隙的形成中扮演了重要的角色。

The relation between stellar chromospheric activity and rotation of evolution stars have a good relativity.

对于介于早F型和M型之间的主序星，色球活动的水平基本上随恒星自转参量的增大而下降。

Between chromospheric activity index and corona activity index of MS stars, there exist good linear relativity.

在第六章中，我们对晚型主序星和演化恒星的色球、冕球磁活动指数的相关性进行分析。

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。

For A-early F type MS stars, stellar chromospheric activity decrease with stellar rotation period, but increase with Rossby number; For M type MS stars, stellar chromospheric activity increase with stellar rotation period and Rossby number, and stellar chromospheric activity reach saturation at large color index; For the MS stars between mid-F to M type, stellar chromospheric activity decrease with stellar rotation period and Rossby number.

在第五章中，我们采用不同的磁活动指数研究了晚型恒星磁活动与恒星自转参量(自转周期、Rossby数)、磁活动与恒星色指数以及恒星磁活动指数之间的相关性。大样本分析显示晚型主序恒星的色球活动与恒星自转参量的研究晚型主序恒星的色球活动与恒星自转参量间的关系表现出对恒星光谱型的依赖。

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 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。

Plunder melds and run with this jewel!

掠夺melds和运行与此宝石！

My dream is to be a crazy growing tree and extend at the edge between the city and the forest.

此刻，也许正是在通往天国的路上，我体验着这白色的晕旋。