发表机构
Space Research Centre, Polish Academy of Sciences; Astronomical Institute, University of Wrocław; ETH-Zürich; PMOD/WRC（波兰科学院空间研究中心; 弗罗茨瓦夫大学天文研究所; 苏黎世联邦理工学院; 帕默尔太阳物理观测站/世界辐射中心）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究利用STIX等数据，发现失败日珥爆发产生三重日冕硬X射线源，其中直接加热源冷却极长，此类源可能普遍存在但较弱。
AI 中文摘要
观测揭示了太阳日冕中形态和位置与典型太阳耀斑不同的硬X射线源。太阳日冕中产生硬X射线（HXR）的一种预期机制是各种类型的爆发。失败的爆发是探测与非耀斑相关HXR源的有前景的目标，因为其大部分能量预计在日冕中耗散。我们研究了SOL2022-0事件，以确定与该事件相关的日冕HXR源的性质。我们使用了Solar Orbiter的STIX、EUI和SDO AIA观测数据。我们使用MARLIN算法重建了STIX图像。我们使用EUI数据从两个有利位置交叉检查事件的视图。AIA图像实现了运动学分析和微分发射测量（DEM）图的重建。然后我们使用AIA DEM预测X射线发射图，并将其与STIX图像进行比较。我们发现了失败爆发与HXR源之间的时间和空间相关性。在日珥爆发的制动过程中，我们观测到沿爆发路径的日冕源发出非热HXR发射。热HXR发射集中在三个日冕源中，这些源通过两种不同的机制形成：色球蒸发和直接加热。直接加热的源是爆发与上方磁场相互作用的结果，并观测到其冷却时间极长。与爆发和上方磁场相互作用相关的HXR发射源可能是所有耀斑中的典型结构。然而，它们看起来较弱，因为其发射仅为耀斑日冕源发射的5-20%。如果足点源未被掩蔽，那么由于HXR望远镜的低动态范围，这些微弱的日冕发射源将不可见。
英文摘要
{Observations reveal hard X-ray sources in the solar corona with morphologies and locations distinct from typical solar flares. One expected mechanisms for hard X-ray (HXR) production in the solar corona is eruptions of various types. Failed eruptions are promising targets for detecting non-flare-related HXR sources because most of their energy is expected to be dissipated in the corona. } {We investigated the SOL2022-0 to determine the nature of coronal HXR sources associated with the event.} {We used Solar Orbiter's STIX, EUI, and SDO AIA observations. We reconstructed STIX images using the MARLIN algorithm. We used EUI data to cross-check the view of the event from two vantage points. The AIA images enabled kinematic analysis and reconstruction of differential emission measure (DEM) maps. We then used the AIA DEM to predict X-ray emission maps and compared them with STIX images. } {We find temporal and spatial correlations between the failed eruption and HXR sources. During the braking of the filament eruption, we observed non-thermal HXR emission from coronal sources along the path of the eruption. Thermal HXR emission was concentrated in three coronal sources formed with two separate mechanisms: chromospheric evaporation and direct heating. Directly heated sources are the result of the interaction of the eruption with the overlying magnetic field, and were observed to cool for an extremely long time.} {The HXR emission sources related to the interaction between the eruption and the overlying magnetic field might be typical structures in all flares. However, they appear to be weak, since their emission is only 5-20~\% of that from the flare coronal source. If footpoint sources were not occulted, then these weak coronal emission sources would not be visible due to the low dynamic range of HXR telescopes.}
CommentsA&A accepted
