Analysis and modeling of high temporal resolution spectroscopic observations of flares on AD Leonis
Analysis and modeling of high temporal resolution spectroscopic observations of flares on AD Leonis
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AD Leonis 耀斑高时间分辨率光谱观测的分析和建模
DOI：
10.1051/0004-6361:20053615
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发表时间：
2006
影响因子：
6.5
通讯作者：
ESTECSCI
中科院分区：
文献类型：
--
作者：
I. Crespo;D. Montes;D. García;M. J. Fernández;J. Lopez;B. Foing;Dept. Astrofisica;Ucm;U. Madrid;H. C. F. Astrophysics;A. Observatory;I. A. D. Palermo;R. Division;Esa Space Science Dept.;ESTECSCI
我们报告了对耀斑恒星AD LEO进行高时间分辨率光谱监测的结果。在4个晚上，使用艾萨克·牛顿望远镜(INT)和中间色散光谱仪(IDS)在光学范围内采集了600多个光谱。我们观察到大量的短而弱的耀斑频繁地出现(耀斑活动>；0.71h^-1)。这与耀斑在恒星日冕加热中扮演的非常重要的角色是一致的。探测到的耀斑是非白光耀斑，尽管大多数太阳耀斑都属于这种类型，但以前在恒星中观察到的此类事件很少。本文详细研究了14个耀斑的不同色球谱线(从H_α到H_11的巴尔默系列、Ca II H&K系列、Na I D_1和D_2系列、He I 4026埃系列和He I D_3系列)的行为。我们使用一种简化的耀斑平板模型来估算耀斑等离子体的物理参数。所有获得的物理参数都与之前导出的恒星耀斑的值一致，并且面积--不到恒星表面的2.3%--与其他太阳和恒星耀斑的推断大小相当。我们研究了物理参数与探测到的耀斑的面积、持续时间、最大通量和能量释放之间的关系。
We report the results of a high temporal resolution spectroscopic monitoring of the flare star AD Leo. During 4 nights, more than 600 spectra were taken in the optical range using the Isaac Newton Telescope (INT) and the Intermediate Dispersion Spectrograph (IDS). We observed a large number of short and weak flares occurring very frequently (flare activity > 0.71 h^-1). This is consistent with the very important role that flares can play in stellar coronal heating. The detected flares are non white-light flares and, although most solar flares are of this kind, very few such events have been observed previously in stars. The behaviour of different chromospheric lines (Balmer series from H_α to H_11, Ca II H & K, Na I D_1 and D_2, He I 4026 angstrom and He i D_3) was studied in detail for a total of 14 flares. We estimated the physical parameters of the flaring plasma by using a procedure that assumes a simplified slab model of flares. All the obtained physical parameters are consistent with previously derived values for stellar flares, and the areas - less than 2.3% of the stellar surface - are comparable with the size inferred for other solar and stellar flares. We studied the relationships between the physical parameters and the area, duration, maximum flux and energy released during the detected flares.