论文标题
中级太阳耀斑中能量沉积层的深度和垂直范围
The depth and the vertical extent of the energy deposition layer in a medium-class solar flare
论文作者
论文摘要
我们在这里分析了C1.6中能量沉积层（EDL）的位置和垂直范围的变化，在2012年9月10日10:20 UT观察到的c1.6级太阳耀斑。EDL的变化与Spopspers coptial s s oss Spects coptial coppart coptial coppart coppart coppart copsect copsect copsect copsect copsect copsect copsect copsect copsect copsect copsect copsect copsect copsect copsect copsect copsect a psoct的变化的变化。 耀斑辐射的硬X射线（HXR）可检测到70 keV的能量。分析中使用的耀斑的数值模型假设非热电子（NTES）将外部能量带到耀斑。 NTES能量通量源自Rhessi光谱中看到的非热成分。使用恢复的Rhessi成像数据得出了耀斑的主要几何参数。 我们发现，在耀斑的前强度和冲动阶段，X射线通量记录的X射线通量的变化与H-Alpha强度的变化良好相关，并且它们同意EDL的计算位置和垂直范围的变化。在H-Alpha线谱的各个部分中注意到的发射的变化是由各个能量沉积物的单个发作引起的，该发作是通过各种能量光谱的NTE的光束在色层等离子体中的各个深度上引起的。这些结果补充了我们先前对2013年6月21日太阳耀斑的发现，几乎相同的C1.1类，但HXR发射仅在34 keV以下（Falewicz等，2017）（以下几点如下）。
We analyze here variations of the position and the vertical extent of the energy deposition layer (EDL) inthe C1.6 GOES-class solar flare observed at 10:20 UT on 2012 September 10. The variations of the EDL arecontrasted with the variations of the spectra and emission intensities recorded in the H-alpha line with the very high time resolution using the MSDP spectrograph at Bialkow Observatory. The flare radiated hard X-rays (HXR) detectable up to a energy of 70 keV. A numerical model of the flare used in the analysis assumes that the non-thermal electrons (NTEs) carried the external energy to the flare. The NTEs energy flux was derived from a non-thermal component seen in RHESSI spectra. The main geometrical parameters of the flare were derived using restored RHESSI imaging data. We found that the variations of the X-ray fluxes recorded in various energy bands and the variations of the H-alpha intensities were well correlated in time during the pre-impulsive and impulsive phases of the flare and they agreed with the variations of the calculated position and vertical extent of the EDL. The variations of the emission noticed in various parts of the H-alpha line profile were caused by individual episodes of energy depositionby the beams of NTEs of various energy spectra on various depths in the chromospheric plasma. These results supplement our previous findings for the solar flare on 21 June2013, having nearly the same GOES-class of C1.1 but HXR emission below 34 keV only (Falewicz et al. 2017) (hereafter Paper I).
