A Statistical Study of Solar White-Light Flares Observed by the White-Light Solar Telescope of the Lyman-Alpha Solar Telescope on the Advanced Space-Based Solar Observatory (ASO-S/LST/WST) at 360 nm

IF 2.7 3区物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS

Solar Physics Pub Date : 2024-01-23 DOI:10.1007/s11207-024-02251-9

Zhichen Jing, Ying Li, Li Feng, Hui Li, Yu Huang, Youping Li, Yang Su, Wei Chen, Jun Tian, Dechao Song, Jingwei Li, Jianchao Xue, Jie Zhao, Lei Lu, Beili Ying, Ping Zhang, Yingna Su, Qingmin Zhang, Dong Li, Yunyi Ge, Shuting Li, Qiao Li, Gen Li, Xiaofeng Liu, Guanglu Shi, Jiahui Shan, Zhengyuan Tian, Yue Zhou, Weiqun Gan

{"title":"A Statistical Study of Solar White-Light Flares Observed by the White-Light Solar Telescope of the Lyman-Alpha Solar Telescope on the Advanced Space-Based Solar Observatory (ASO-S/LST/WST) at 360 nm","authors":"Zhichen Jing, Ying Li, Li Feng, Hui Li, Yu Huang, Youping Li, Yang Su, Wei Chen, Jun Tian, Dechao Song, Jingwei Li, Jianchao Xue, Jie Zhao, Lei Lu, Beili Ying, Ping Zhang, Yingna Su, Qingmin Zhang, Dong Li, Yunyi Ge, Shuting Li, Qiao Li, Gen Li, Xiaofeng Liu, Guanglu Shi, Jiahui Shan, Zhengyuan Tian, Yue Zhou, Weiqun Gan","doi":"10.1007/s11207-024-02251-9","DOIUrl":null,"url":null,"abstract":"<div>Solar white-light flares (WLFs) are those accompanied by brightenings in the optical continuum or integrated light. The White-light Solar Telescope (WST), as an instrument of the Lyman-alpha Solar Telescope (LST) on the Advanced Space-based Solar Observatory (ASO-S), provides continuous solar full-disk images at 360 nm, which can be used to study WLFs. We analyze 205 major flares above M1.0 from October 2022 to May 2023 and identify 49 WLFs at 360 nm from WST observations, i.e. with an occurrence rate of 23.9%. The percentages of WLFs for M1 – M4 (31 out of 180), M5 – M9 (11 out of 18), and above X1 (7 for all) flares are 17.2%, 61.1%, and 100%, respectively, namely the larger the flares, the more likely they are WLFs at 360 nm. We further analyze 39 WLFs among the identified WLFs and investigate their properties such as white-light enhancement, duration, and brightening area. It is found that the relative enhancement of the white-light emission at 360 nm is mostly (>90%) less than 30% and the mean enhancement is 19.4%. The WLFs’ duration at 360 nm is mostly (>80%) less than 20 minutes and its mean is 10.3 minutes. The brightening area at 360 nm is mostly (>75%) less than 500 arcsecond2 and the median value is 225. We find that there exist good correlations between the white-light enhancement/duration/area and the peak soft X-ray (SXR) flux of the flare, with correlation coefficients of 0.68, 0.58, and 0.80, respectively. In addition, the white-light emission in most WLFs peaks around the same time as the temporal derivative of SXR flux as well as the hard X-ray emission at 20 – 50 keV, indicative of the Neupert effect. It is also found that the limb WLFs are more likely to have a greater enhancement, which is consistent with numerical simulations.</div>","PeriodicalId":777,"journal":{"name":"Solar Physics","volume":null,"pages":null},"PeriodicalIF":2.7000,"publicationDate":"2024-01-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s11207-024-02251-9.pdf","citationCount":"0","resultStr":null,"platform":"Semanticscholar","paperid":null,"PeriodicalName":"Solar Physics","FirstCategoryId":"101","ListUrlMain":"https://link.springer.com/article/10.1007/s11207-024-02251-9","RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"Q2","JCRName":"ASTRONOMY & ASTROPHYSICS","Score":null,"Total":0}

引用次数: 0

Abstract

Solar white-light flares (WLFs) are those accompanied by brightenings in the optical continuum or integrated light. The White-light Solar Telescope (WST), as an instrument of the Lyman-alpha Solar Telescope (LST) on the Advanced Space-based Solar Observatory (ASO-S), provides continuous solar full-disk images at 360 nm, which can be used to study WLFs. We analyze 205 major flares above M1.0 from October 2022 to May 2023 and identify 49 WLFs at 360 nm from WST observations, i.e. with an occurrence rate of 23.9%. The percentages of WLFs for M1 – M4 (31 out of 180), M5 – M9 (11 out of 18), and above X1 (7 for all) flares are 17.2%, 61.1%, and 100%, respectively, namely the larger the flares, the more likely they are WLFs at 360 nm. We further analyze 39 WLFs among the identified WLFs and investigate their properties such as white-light enhancement, duration, and brightening area. It is found that the relative enhancement of the white-light emission at 360 nm is mostly (>90%) less than 30% and the mean enhancement is 19.4%. The WLFs’ duration at 360 nm is mostly (>80%) less than 20 minutes and its mean is 10.3 minutes. The brightening area at 360 nm is mostly (>75%) less than 500 arcsecond² and the median value is 225. We find that there exist good correlations between the white-light enhancement/duration/area and the peak soft X-ray (SXR) flux of the flare, with correlation coefficients of 0.68, 0.58, and 0.80, respectively. In addition, the white-light emission in most WLFs peaks around the same time as the temporal derivative of SXR flux as well as the hard X-ray emission at 20 – 50 keV, indicative of the Neupert effect. It is also found that the limb WLFs are more likely to have a greater enhancement, which is consistent with numerical simulations.

Abstract Image

查看原文本刊更多论文

先进天基太阳观测站莱曼-阿尔法太阳望远镜（ASO-S/LST/WST）的白光太阳望远镜在 360 纳米波长观测到的太阳白光耀斑的统计研究

太阳白光耀斑（WLF）是指伴随着光学连续面或综合光的增亮的耀斑。白光太阳望远镜（WST）是先进天基太阳观测站（ASO-S）上莱曼-阿尔法太阳望远镜（LST）的一个仪器，可提供360纳米波长的连续太阳全盘图像，可用于研究WLF。我们分析了2022年10月至2023年5月期间的205个M1.0以上的大耀斑，并从WST的观测中发现了49个360纳米波长的WLF，即发生率为23.9%。M1-M4（180颗中有31颗）、M5-M9（18颗中有11颗）和X1以上（全部7颗）耀斑的WLF比例分别为17.2%、61.1%和100%，即耀斑越大，越有可能是360纳米波段的WLF。我们进一步分析了已识别 WLF 中的 39 个 WLF，并研究了它们的特性，如白光增强、持续时间和增亮面积。结果发现，360 nm 处白光发射的相对增强率大多（90%）小于 30%，平均增强率为 19.4%。360 纳米波长的 WLFs 持续时间大多（>80%）小于 20 分钟，平均为 10.3 分钟。360 纳米波段的增亮面积大多（75%）小于 500 弧秒2，中值为 225。我们发现耀斑的白光增强/持续时间/面积与软 X 射线（SXR）通量峰值之间存在良好的相关性，相关系数分别为 0.68、0.58 和 0.80。此外，大多数 WLF 的白光发射与 SXR 通量的时间导数以及 20-50 keV 的硬 X 射线发射在同一时间达到峰值，这表明存在 Neupert 效应。研究还发现，边缘 WLFs 更有可能有更大的增强，这与数值模拟结果是一致的。

本文章由计算机程序翻译，如有差异，请以英文原文为准。

求助全文

约1分钟内获得全文求助全文

来源期刊

Solar Physics 地学天文-天文与天体物理

CiteScore

5.10

自引率

17.90%

发文量

146

审稿时长

1 months

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.