色球

基本解释 (translations)

chromosphere

与色球相关的网络例句 [注：此内容来源于网络，仅供参考]

Chromosphere 色球层 A layer of the Sun which is above the photosphere , and it appears red in colour.

在太阳光球外面的一层，呈红色。

Besides, we also discussed the instability of shock wave, the differences between thermal model and non-thermal model, chromospheric cendensation and comparisons with the observations.

文中并就环顶激波的不稳定性、热模型和非热模型的大气演化差异、热模型下色球加热的可能性、色球压缩区的性质、以及与其它模型相比较等方面进行了讨论。

From the distribution of rotation period and convection parameter of M type stars, stellar chromospheric activity of M type stars depart from the anticipation of a.

对于A—早F型主序恒星的色球活动水平也随自转周期呈线性下降趋势，随Rossby数却呈上升趋势。A—早F型主序恒星的自转周期和恒星对流区的随色指数的分布明显地影响着这些恒星的色球活动行为。

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。

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。

In the frame of constructing hydrodynamical model, some basic assumptions and equations were described in detail. Besides, there are three distinguish improvements above the former work: a new formula of chromosphere radiative loss was deduced out, which can roughly reproduce the results calculated by detailed non-LTE theory; a new physical process, i.e.

在构造耀斑动力学模型理论框架中，我们详细交待了基本假设和基本方程组，以及方程中各项的选取情况；针对现有耀斑动力学模型色球研究的不足，文中导得了新的色球辐射损失经验公式，它基本能够再生现有详细非局部热动平衡计算结果，较以前的处理方法有很大程度上的改善；引入了以前在耀斑环研究中从未被考虑过的日冕软x辐射加热色球的能量过程，推得了日冕软x辐射色球沉积的自恰公式。

We produced by the elastic rubber ball is high-quality synthetic rubber made include: three-dimensional of the ball, the ball picture, the electronic ball, the ball modeling, three-dimensional King of the ball deep, luminous ball, the ball monochrome, multicolor Ball, the ball printed in Pictures, a key hammer, magnet ball, water polo, with a large bounce of.

我们所生产的橡胶弹力球是由高品质的合成橡胶制成，种类包括：立体物球，图片球，电子球，造型球，深景立体物球，夜光球，单色球，多色球，剪影印刷球，钥匙链球，磁铁球，水球等，具有相当大的弹跳性。

与色球相关的网络解释 [注：此内容来源于网络，仅供参考]

chromospheric facula：色球光斑

chromospheric evaporation 色球蒸发 | chromospheric facula 色球光斑 | chromospheric fine structure 色球精细结构

chromospheric flocculus：色球谱斑

chromospheric eruption 耀斑;色球爆发 | chromospheric flocculus 色球谱斑 | chromospheric mottling 色球日芒

chromospheric mottling：色球日芒

chromospheric flocculus 色球谱斑 | chromospheric mottling 色球日芒 | chromospheric network 色球网络

chromospheric matirial：色球物质

chromospheric line 色球谱线 | chromospheric matirial 色球物质 | chromospheric spectrum 色球光谱

chromospheric activity：色球活动

chromosphere-corona transition zone 色球-日冕过渡层 | chromospheric activity 色球活动 | chromospherically active banary 色球活动双星

chromospheric line：色球谱线

chromospherically active star 色球活动星 | chromospheric line 色球谱线 | chromospheric matirial 色球物质

Chroococcaceae：色球藻科(藍)

色帶;色譜 chromatogram | 色球藻科(藍) Chroococcaceae | 色球藻目(藍) Chroococcales

Chroococcales：色球藻目(藍)

色球藻科(藍) Chroococcaceae | 色球藻目(藍) Chroococcales | 色球藻型的 chroococcoid

chroococcoid：色球藻型的

色球藻目(藍) Chroococcales | 色球藻型的 chroococcoid | 色球藻屬(藍) Chroococcus

Chroococcus：色球藻

色球藻 色球藻(Chroococcus) 蓝藻门、色球藻科. 藻体多数为2、4、6或更多一些细胞组成的群体,少数为单细胞. 单细胞时细胞球形,群体中的细胞为半球形或四分之一圆形. 细胞均具明显胶见"耀斑". 色球爆发在百度百科中为本词条的同义词,