Magnetic Field Evolution of the Solar Active Region 13664

Robert Jarolim, Astrid M. Veronig, Stefan Purkhart, Peijin Zhang and Matthias Rempel
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Abstract

On 2024 May 10–11, the strongest geomagnetic storm since 2003 November occurred, with a peak Dst index of −412 nT. The storm was caused by NOAA active region (AR) 13664, which was the source of a large number of coronal mass ejections and flares, including 12 X-class flares. Starting from about May 7, AR 13664 showed a steep increase in its size and (free) magnetic energy, along with increased flare activity. In this study, we perform 3D magnetic field extrapolations with the NF2 nonlinear force-free code based on physics-informed neural networks (R. Jarolim et al.). In addition, we introduce the computation of the vector potential to achieve divergence-free solutions. We extrapolate vector magnetograms from the Solar Dynamics Observatory’s Helioseismic and Magnetic Imager at the full 12 minute cadence from 2024 May 5 00:00 to 11 04:36 UT, in order to understand the AR’s magnetic evolution and the large eruptions it produced. A decrease in the calculated relative free magnetic energy can be related to solar flares in ∼90% of the cases, and all considered X-class flares are reflected by a decrease in the relative free magnetic energy. Regions of enhanced free magnetic energy and depleted magnetic energy between the start and end times of major X-class flares show spatial alignment with brightness increases in extreme-ultraviolet observations. We provide a detailed analysis of the X3.9-class flare on May 10, where we show that the interaction between separated magnetic domains is directly linked to major flaring events. With this study, we provide a comprehensive data set of the magnetic evolution of AR 13664 and make it publicly available for further analysis.
太阳活动区 13664 的磁场演变
2024 年 5 月 10-11 日,发生了自 2003 年 11 月以来最强的地磁暴,峰值 Dst 指数为 -412 nT。这场风暴是由美国国家海洋和大气管理局活动区(AR)13664 引起的,该活动区是大量日冕物质抛射和耀斑的源头,其中包括 12 个 X 级耀斑。大约从 5 月 7 日开始,AR 13664 的大小和(自由)磁能急剧增加,耀斑活动也随之增加。在这项研究中,我们利用基于物理信息神经网络的 NF2 非线性无作用力代码(R. Jarolim 等人)进行了三维磁场外推。此外,我们还引入了矢量势的计算,以实现无发散求解。我们推断了太阳动力学天文台的日震和磁成像仪从 2024 年 5 月 5 日 00:00 到 11 日 04:36 (美国东部标准时间)整个 12 分钟周期的矢量磁图,以了解 AR 的磁演化及其产生的大爆发。计算出的相对自由磁能的减少在90%的情况下与太阳耀斑有关,所有被考虑的X级耀斑都反映了相对自由磁能的减少。在主要的 X 级耀斑开始和结束时间之间的自由磁能增强区和磁能耗竭区在空间上与极紫外观测的亮度增加一致。我们对5月10日的X3.9级耀斑进行了详细分析,结果表明分离磁畴之间的相互作用与主要耀斑事件直接相关。通过这项研究,我们提供了 AR 13664 磁演化的全面数据集,并将其公开,以供进一步分析。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
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