Spectral and Imaging Observations of a C2.3 White-Light Flare from the Advanced Space-Based Solar Observatory (ASO-S) and the Chinese H$α$ Solar Explorer (CHASE)
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| Autores principales: | , , , , , , , , , , , , , , , , , , , , , , , , , , , , , |
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| Formato: | Preprint |
| Publicado: |
2024
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| author | Li, Qiao Li, Ying Su, Yang Song, Dechao Li, Hui Feng, Li Huang, Yu Li, Youping Li, Jingwei Zhao, Jie Lu, Lei Ying, Beili Xue, Jianchao Zhang, Ping Tian, Jun Liu, Xiaofeng Li, Gen Jing, Zhichen Li, Shuting Shi, Guanglu Tian, Zhengyuan Chen, Wei Su, Yingna Zhang, Qingmin Li, Dong Ge, Yunyi Shan, Jiahui Zhou, Yue Lei, Shijun Gan, Weiqun |
| author_facet | Li, Qiao Li, Ying Su, Yang Song, Dechao Li, Hui Feng, Li Huang, Yu Li, Youping Li, Jingwei Zhao, Jie Lu, Lei Ying, Beili Xue, Jianchao Zhang, Ping Tian, Jun Liu, Xiaofeng Li, Gen Jing, Zhichen Li, Shuting Shi, Guanglu Tian, Zhengyuan Chen, Wei Su, Yingna Zhang, Qingmin Li, Dong Ge, Yunyi Shan, Jiahui Zhou, Yue Lei, Shijun Gan, Weiqun |
| contents | Solar white-light flares are characterized by an enhancement in the optical continuum, which are usually large flares (say X- and M-class flares). Here we report a small C2.3 white-light flare (SOL2022-12-20T04:10) observed by the \emph{Advanced Space-based Solar Observatory} and the \emph{Chinese H$α$ Solar Explorer}. This flare exhibits an increase of $\approx$6.4\% in the photospheric Fe \textsc{i} line at 6569.2\,Å and {$\approx$3.2\%} in the nearby continuum. The continuum at 3600\,Å also shows an enhancement of $\approx$4.7\%. The white-light brightening 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 brightening kernels, the Fe \textsc{i} line displays an absorption profile that has a good Gaussian shape, with a redshift up to $\approx$1.7 km s$^{-1}$, while the H$α$ line shows an emission profile though having a central reversal. The H$α$ 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$α$ asymmetry is opposite at the conjugate footpoints. It is also found that the CHASE continuum increase seems to be related to the change of 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. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2405_01308 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Spectral and Imaging Observations of a C2.3 White-Light Flare from the Advanced Space-Based Solar Observatory (ASO-S) and the Chinese H$α$ Solar Explorer (CHASE) Li, Qiao Li, Ying Su, Yang Song, Dechao Li, Hui Feng, Li Huang, Yu Li, Youping Li, Jingwei Zhao, Jie Lu, Lei Ying, Beili Xue, Jianchao Zhang, Ping Tian, Jun Liu, Xiaofeng Li, Gen Jing, Zhichen Li, Shuting Shi, Guanglu Tian, Zhengyuan Chen, Wei Su, Yingna Zhang, Qingmin Li, Dong Ge, Yunyi Shan, Jiahui Zhou, Yue Lei, Shijun Gan, Weiqun Solar and Stellar Astrophysics Solar white-light flares are characterized by an enhancement in the optical continuum, which are usually large flares (say X- and M-class flares). Here we report a small C2.3 white-light flare (SOL2022-12-20T04:10) observed by the \emph{Advanced Space-based Solar Observatory} and the \emph{Chinese H$α$ Solar Explorer}. This flare exhibits an increase of $\approx$6.4\% in the photospheric Fe \textsc{i} line at 6569.2\,Å and {$\approx$3.2\%} in the nearby continuum. The continuum at 3600\,Å also shows an enhancement of $\approx$4.7\%. The white-light brightening 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 brightening kernels, the Fe \textsc{i} line displays an absorption profile that has a good Gaussian shape, with a redshift up to $\approx$1.7 km s$^{-1}$, while the H$α$ line shows an emission profile though having a central reversal. The H$α$ 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$α$ asymmetry is opposite at the conjugate footpoints. It is also found that the CHASE continuum increase seems to be related to the change of 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. |
| title | Spectral and Imaging Observations of a C2.3 White-Light Flare from the Advanced Space-Based Solar Observatory (ASO-S) and the Chinese H$α$ Solar Explorer (CHASE) |
| topic | Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2405.01308 |