Abstract—

The results from the analysis of spectral observations in the Hα line of the active region (AR) NOAA 11024, in which the Ellerman bomb (EB) and various chromospheric surges developed, are presented. Spectral data with high spatial and temporal resolution were obtained using the THEMIS French–Italian solar telescope (Tenerife, Spain) on July 4, 2009. The observation time was 20 min. On the day of the observations, the AR was at the stage of a sharp increase in activity. The Hα line profiles obtained for different periods of the Ellerman bomb development were very diverse, mainly consisted of several components, and were asymmetrical with excess emission in the short-wavelength wing. The maximum increase in the intensity of the emission component, compared with the profile for the AR segment without active formations, in the short-wavelength wing by 73% and in the long-wavelength wing by 35% occurred at a distance of ±0.16 nm from the core of the Hα line. The temporal variations of intensity in the wings of the Hα line indicate that there was a gradual energy release for the first 8 min of the Ellerman bomb development and then there was a pulse energy release for 6 min. The EB brightness increase period consisted of five peaks with an interval of approximately 1 min. The obtained temporal changes in the line-of-sight velocity (V_los) of the chromospheric matter over the EB development region at the level of the Hα line core formation indicate that the velocity distribution in this region was mainly due to the development of chromospheric surges. In the segment without active formations, values of V_los experienced small fluctuations within ±2 km/s. Two periods of increase in V_los are distinguished. They consisted of several individual peaks: in the first half of the observations, the chromospheric matter mainly moved upward, while it mainly moved downward in the second half of the observations. Above the EB development region, different kinds of Hα-surges were observed. The maximum upward velocity in the return surges reached –12 to –16 km/s and the chromospheric matter descended along the same trajectories of magnetic loops with two times higher velocity, up to 22–30 km/s. In the loop surge, the maximum upward velocity on one side of the loop was –7 km/s and the downward velocity on the other side reached 18 km/s. One of the surges showed signs of plasma vortex motions, as evidenced by the inclined dark streaks in the spectra. Features of intensity variation in the wings of the Hα line and in the line-of-sight velocity of the chromospheric matter indicate that the Ellerman bomb and the accompanying Hα-surges, which appeared and developed in the AR under study, resulted from the magnetic reconnection caused by the emergence of the new serpentine magnetic flux and its interaction with the pre-existing magnetic field or between the magnetic loops of the flux itself.

中文翻译：

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Ellerman炸弹和Hα激增对有效区域的光谱研究。大气层。埃勒曼炸弹

摘要-

给出了对活动区域（AR）NOAA 11024的Hα线的光谱观测结果的分析结果，其中出现了Ellerman炸弹（EB）和各种色球涌动。2009年7月4日，使用THEMIS法国-意大利太阳望远镜（西班牙特内里费岛）获得了具有高时空分辨率的光谱数据。观测时间为20分钟。在观察当天，AR处于活动急剧增加的阶段。在Ellerman炸弹发展的不同时期获得的Hα谱线非常多样化，主要由几个组成部分组成，并且在短波长机翼中具有不对称的过量发射。与没有活跃地层的AR段的剖面相比，发射分量强度的最大增加，在距Hα线核心±0.16 nm处发生的短波翼中占73％，长波翼中占35％。Hα线机翼强度的时间变化表明，在Ellerman炸弹发展的最初8分钟内能量逐渐释放，然后在6分钟内脉冲能量释放。EB亮度增加周期由五个峰组成，每个峰的间隔约为1分钟。获得的视线速度的时间变化（EB亮度增加周期由五个峰组成，每个峰的间隔约为1分钟。获得的视线速度的时间变化（EB亮度增加周期由五个峰组成，每个峰的间隔约为1分钟。获得的视线速度的时间变化（在EB发育区域上处于Hα线核心形成水平的色球物质的V _los）表明，该区域的速度分布主要是由于色球涌动的发展所致。在没有活跃地层的段中，V _los的值在±2 km / s之内经历了小的波动。V _los增加两个时期杰出。它们由几个单独的峰组成：在观测的前半部分，色球物质主要向上移动，而在观测的后半部分则主要向下移动。在EB发育区域上方，观察到了不同类型的Hα浪涌。回波的最大上升速度达到–12至–16 km / s，色球物质沿着相同的磁环轨迹下降，速度最高时达到22–30 km / s，是原来的两倍。在环路涌动中，环路一侧的最大上行速度为–7 km / s，另一侧的下行速度达到18 km / s。波峰之一显示出等离子体涡旋运动的迹象，如频谱中倾斜的暗条纹所证明。