查询词典 chromospheric

Line and pumping by chromospheric CII 1037.0182 ?

线存在Doppler变暗，以及来自色球层CII 1037.0182 ？

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。

Abundances of Li versus chromospheric activity indices 17, RHK, for the solar analogue stars with and without detected planets are shown in Fig.

在图表2a中，对于&类太阳&恒星中的&有行星&恒星以及&无行星&恒星，用Rhk来表示锂丰度相对色球层活动指数（参考文献17）。

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。

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 detailed time-match semiempirical models represnting the chromospheric state during the impulsive phase of the 2B flare on Fab. 3 1983 are proposed by making the non-LTE calculstions on hydrogen and ionized calcium. The physical pictures of total evolutionary pattern of the impulsivs phase of the flare are improved either quantitatively or qualitatively in comparison with the former work we did.

利用南京大学太阳塔多波段光谱仪拍摄到的1983年2月3日2B级耀斑脉冲相期间的Hα和CaⅡK线轮廓系列光谱资料，按照我们所发展的构造定态色球耀斑半经验模型的方法，通过联立求解氢和一次电离钙的能级平衡方程和辐射转移方程，建立了能够再生Hα和CaⅡK线观测轮廓的更为完整的1983年2月3日2B级耀斑脉冲相色球半经验模型。

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。

Finally, according to market conditions and market products this article paper analyzes the trends in the development of camera technology, and designs a color night vision camera.

最后根据市场情况和市面上产品的情况分析了摄像机技术的发展趋势，并设计了一款彩色夜视摄像机。

Only person height weeds and the fierce looks stone idles were there.

只有半人深的荒草和龇牙咧嘴的神像。