chromosphere ['krəuməsfiə]

chromosphere的基本解释

n.

色球, 太阳的色球层

与chromosphere相关的网络例句 [注：此内容来源于网络，仅供参考]

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。

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。

Soon , it is not enough to make again , combine with the brown chromosphere and blue chromosphere.

不久，又赚不够，再加上了棕色球和蓝色球。

与chromosphere相关的网络解释 [注：此内容来源于网络，仅供参考]

chromosphere：色球

这薄气层就叫做"色球"(chromosphere),因为它有和日珥一样的深红色--从这一点可以得知,同日珥一样,色球由和日珥基本类似的元素组成,其主要成分也是氢.

chromosphere：色球层

一般认为 闪焰耀斑 是发生在 色球层 (Chromosphere) 中,所以也称它为「 色球爆发 」. 在天文望远镜中观看 闪焰耀斑 的表现,它只是一个突然出现并迅速剧增亮度的亮点. 别小看它的初线仅是一个小亮点,一旦 闪焰耀斑 出现,简直是一次惊天动地的大爆发.

chromosphere：色层球

chromoscopechromosome 染色体 | chromosphere 色层球 | chromotron flter 光谱性质识别滤光器

chromosphere：色層;太陽

"chromium plating","镀铬" | "chromosphere","色层;太阳" | "chronograph","记时器;马表"

upper chromosphere：色球高层

这条光谱线上的放射物是温度高达10万华氏度的色球高层(upper chromosphere). 照片中的每一个特征都追寻着磁场结构的足迹. 温度最高的区域几乎全是白色,而颜色暗红的区域则表明温度相对较低. 2.太阳表面磁场结构的特写太阳表面磁场结构的特写 这是一张有关太阳表面磁场结构的特写照片,