Hα Impact Polarization Observed in a Gradual Flare
Hα Impact Polarization Observed in a Gradual Flare
复制标题
在渐变耀斑中观察到的 Hα 撞击极化
DOI：
10.1086/378123
复制
发表时间：
2003
期刊：
影响因子：
--
通讯作者：
Y. Hanaoka
中科院分区：
文献类型：
--
作者：
Y. Hanaoka
在一个渐变的耀斑核中检测到Hα线的线偏振，并伴有长丝喷发。该耀斑的最大极化度超过1%，极化方向近似垂直于耀斑带。这些结果可以用观测到的极化是由加速质子产生的冲击极化的假设来解释。还观察到耀斑核的Hα发射层向下运动，这通常被认为是对色球蒸发的反应。在核增亮上升阶段，极化和向下运动都表现出明显的信号。这一事实表明，不仅是向下运动，而且偏振也与色球的加热剂密切相关。Reuven Ramaty高能太阳光谱成像仪（RHESSI）观察到的硬x射线显示出热成分，但由于加速电子，没有可检测到的幂律成分。因此，质子被认为不仅是极化的原因，而且可能是这个耀斑中主要加热剂的候选者，它缺乏高能电子。
Linear polarization of the Hα line was detected in kernels of a gradual flare, which was accompanied by a filament eruption. The maximum degree of polarization of this flare exceeds 1%, and the orientation of the polarization is approximately perpendicular to the flare ribbons. These results can be explained with the assumption that the observed polarization is impact polarization produced by accelerated protons. Downward motion of the Hα emitting layer of the flare kernels, which is generally accepted as the reaction to the chromospheric evaporation, was also observed. Both the polarization and the downward motion show the tendency to exhibit a significant signal during the rise phase of kernel brightenings. This fact suggests that not only the downward motion but also the polarization is closely related to the heating agent of the chromosphere. The hard X-rays observed by the Reuven Ramaty High-Energy Solar Spectroscopic Imager (RHESSI) show a thermal component, but there is no detectable power-law component due to accelerated electrons. Therefore, protons are presumed to be not only the cause of the polarization but also a possible candidate of the principal heating agent in this flare, which lacks high-energy electrons.