Spectral and Imaging Observations of a C2.3 White-Light Flare from the Advanced Space-Based Solar Observatory (ASO-S) and the Chinese H\(\alpha \) Solar Explorer (CHASE)
Qiao Li, Ying Li, Yang Su, Dechao Song, Hui Li, Li Feng, Yu Huang, Youping Li, Jingwei Li, Jie Zhao, Lei Lu, Beili Ying, Jianchao Xue, Ping Zhang, Jun Tian, Xiaofeng Liu, Gen Li, Zhichen Jing, Shuting Li, Guanglu Shi, Zhengyuan Tian, Wei Chen, Yingna Su, Qingmin Zhang, Dong Li, Yunyi Ge, Jiahui Shan, Yue Zhou, Shijun Lei, Weiqun Gan
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引用次数: 0
Abstract
Solar white-light flares are characterized by an enhancement in the optical continuum, which are usually large flares (X- and M-class flares). Here, we report a small C2.3 white-light flare (SOL2022-12-20T04:10) observed by the Advanced Space-based Solar Observatory and the Chinese H\(\alpha \)Solar Explorer (CHASE). This flare exhibits an increase of ≈ 6.4% in the photospheric Fe i line at 6569.2 Å and ≈ 3.2% in the nearby continuum. The continuum at 3600 Å also shows an enhancement of ≈ 4.7%. The white-light bright kernels are mainly located at the flare ribbons and co-spatial with nonthermal hard X-ray sources, which implies that the enhanced white-light emissions are related to nonthermal electron-beam heating. At the bright kernels, the Fe i line displays an absorption profile that has a good Gaussian shape, with a redshift up to ≈ 1.7 km s−1, while the H\(\alpha \) line shows an emission profile having a central reversal. The H\(\alpha \) line profile also shows a red or blue asymmetry caused by plasma flows with a velocity of several to tens of km s−1. It is interesting to find that the H\(\alpha \) asymmetry is opposite at the conjugate footpoints. It is also found that the CHASE continuum increase seems to be related to the change in the photospheric magnetic field. Our study provides comprehensive characteristics of a small white-light flare that help understand the energy release process of white-light flares.
太阳白光耀斑的特征是光学连续面的增强，通常是大耀斑（X级和M级耀斑）。在这里，我们报告了先进天基太阳观测站和中国H（α）太阳探测器（CHASE）观测到的一个小型C2.3白光耀斑（SOL2022-12-20T04:10）。该耀斑在6569.2埃处的光球Fe i线上升了≈6.4%，在附近的连续相中上升了≈3.2%。3600 Å 处的连续波也显示出≈ 4.7% 的增强。白光亮核主要位于耀斑带，与非热硬质 X 射线源同空间，这意味着增强的白光辐射与非热电子束加热有关。在亮核处，Fe i线显示出具有良好高斯形状的吸收曲线，红移可达≈ 1.7 km s-1，而H（α）线显示出具有中心反转的发射曲线。H（α）线剖面还显示出红色或蓝色的不对称，这是由速度为几千米/秒到几十千米/秒的等离子体流引起的。有趣的是，在共轭脚点，H（α）线的不对称是相反的。研究还发现，CHASE连续波的增加似乎与光球磁场的变化有关。我们的研究提供了小型白光耀斑的综合特征，有助于理解白光耀斑的能量释放过程。
期刊介绍：
Solar Physics was founded in 1967 and is the principal journal for the publication of the results of fundamental research on the Sun. The journal treats all aspects of solar physics, ranging from the internal structure of the Sun and its evolution to the outer corona and solar wind in interplanetary space. Papers on solar-terrestrial physics and on stellar research are also published when their results have a direct bearing on our understanding of the Sun.
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