arXiv 1710.040672017-10-11astro-ph.SR

C3太阳耀斑中的H $α$和H $β$发射：观测和模拟之间的比较

H$α$ and H$β$ emission in a C3.3 solar flare: comparison between observations and simulations

Vincenzo Capparelli, Francesca Zuccarello, Paolo Romano, Paulo J. A. Simoes, Lyndsay Fletcher, David Kuridze, Mihalis Mathioudakis, Peter H. Keys, Gianna Cauzzi, Mats Carlsson

备注：: 14 pages, 17 figures
DOI：: 10.3847/1538-4357/aa9187

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摘要：

氢巴耳末系是耀斑期间太阳色球层的一个基本辐射损失通道。我们在这里报告的分析一个非常罕见的同时观测的太阳耀斑在H $α$和H $β$线在高空间和时间分辨率，这是在邓恩太阳望远镜获得。利用干涉二维光谱仪（IBIS）沿H $α$谱线剖面和H $β$利用太阳大气快速振荡（ROSA）宽带成像仪拍摄的C3.3耀斑（SOL 2014 -04- 22 T15：22）的不同波长图像，分析了耀斑的强度演化。在三个确定的耀斑足点中H $α$和H $β$强度过度在时间上具有良好的相关性。我们检查了H $α$与H $β$耀斑过量的比率，这是由之前的作者提出的，作为电子束能量输入水平的可能诊断。在较强的足点，H $α$ /H $β$强度比的典型值观察到的是$\sim 0.4-0.5$，在广泛的协议从一个RADYN非LTE模拟驱动的电子束参数约束（尽可能）的观察值。较弱的足点具有较大的H $α$ /H $β$比，同样与RADYN模拟一致，但具有较小的能量通量。所观察到的H $α$谱线的中心反转比RADYN结果所预测的要小，但如果H $α$发射材料的填充因子约为0.2- 0.3，则可以达成一致。

英文摘要：

The Hydrogen Balmer series is a basic radiative loss channel from the flaring solar chromosphere. We report here on the analysis of an extremely rare set of simultaneous observations of a solar flare in the H$α$ and H$β$ lines at high spatial and temporal resolution, which were acquired at the Dunn Solar Telescope. Images of the C3.3 flare (SOL2014-04-22T15:22) made at various wavelengths along the H$α$ line profile by the Interferometric Bidimensional Spectrometer (IBIS) and in the H$β$ with the Rapid Oscillations in the Solar Atmosphere (ROSA) broadband imager are analyzed to obtain the intensity evolution. The H$α$ and H$β$ intensity excesses in three identified flare footpoints are well correlated in time. We examine the ratio of H$α$ to H$β$ flare excess, which was proposed by previous authors as a possible diagnostic of the level of electron beam energy input. In the stronger footpoints, the typical value of the the H$α$/H$β$ intensity ratio observed is $\sim 0.4-0.5$, in broad agreement with values obtained from a RADYN non-LTE simulation driven by an electron beam with parameters constrained (as far as possible) by observation. The weaker footpoint has a larger H$α$/H$β$ ratio, again consistent with a RADYN simulation but with a smaller energy flux. The H$α$ line profiles observed have a less prominent central reversal than is predicted by the RADYN results, but can be brought into agreement if the H$α$-emitting material has a filling factor of around 0.2--0.3.

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