Core Insights - The Daniel K. Inouye Solar Telescope has captured the clearest images of solar flares to date at H-α wavelength (656.28 nm), marking a significant advancement in solar observation [1][2] - The telescope recorded numerous dark coronal loops during an X1.3-class flare, with an average width of 48.2 kilometers and a minimum width of 21 kilometers, setting a record for the narrowest coronal loops observed [1] - This breakthrough allows scientists to directly study the fundamental processes driving flares, such as magnetic reconnection, which were previously only theorized [1] Group 1 - The Inouye Telescope's observations provide a direct view of coronal loops, which are plasma arcs along solar magnetic field lines, often appearing before flares [1] - The ability to observe these structures at such a fine scale enables researchers to investigate the core mechanisms behind flare occurrences [1][2] - The imagery produced by the telescope is described as stunning, with dark filamentous loops resembling a glowing archway, allowing even non-experts to appreciate the complexity and beauty of solar phenomena [2] Group 2 - The previous theoretical predictions suggested that the width of these loops could range from 10 kilometers to 100 kilometers, but direct observation was hindered by resolution limitations [1] - The Inouye Telescope's capability to capture these details represents a leap forward in solar physics, providing insights that were previously confined to theoretical models [1] - The findings may have implications for understanding solar storms and their potential impact on Earth's critical infrastructure [1]

来源：科技日报 科技日报北京8月26日电（记者 张佳欣）据《天体物理学杂志快报》25日报道，美国国家科学基金会丹 尼尔·井上太阳望远镜首次以H-α波长（656.28纳米）拍摄到迄今最清晰的太阳耀斑图像。同时，望远镜 在一次X1.3级耀斑的衰减阶段记录下大量暗色回路。这些回路平均宽度48.2公里，最细仅21公里，创下 了人类观测到的最窄日冕回路纪录。这一突破让科学家得以窥见太阳日冕回路的基本单元，也把耀斑建 模推进一个全新境界。 在井上望远镜之前，人们只能想象这种尺度图案的景象，现在科学家终于能够直接观测到。这也是井上 望远镜首次捕捉到X级耀斑。 日冕回路是沿太阳磁力线分布的等离子体弧拱，常常出现在耀斑之前。当部分磁力线发生扭曲并断裂 时，会释放出巨大能量，引发太阳风暴并影响地球关键基础设施。此前，理论预测这些回路的宽度可能 在10公里至100公里之间，但由于分辨率限制，长期以来无法得到直接验证。井上望远镜的观测首次揭 示了如此清晰的结构，意味着科学家能在此前仅在理论模型中存在的尺度，直接研究磁重联等驱动耀斑 的基本过程，有望揭示耀斑发生的核心机制。 这些细丝状回路可能就是耀斑的基本构件。如果这一推测成立，意味 ...

Core Insights - The Parker Solar Probe has achieved the first direct observation of magnetic reconnection in the solar atmosphere, confirming a theory proposed 70 years ago, which enhances the ability to predict solar storms [1][2] - Magnetic reconnection is a process where magnetic field lines break and reconnect, releasing significant magnetic energy, which can lead to solar flares and coronal mass ejections [1] - The successful observation was made possible by the Parker Solar Probe's close approach to the Sun and collaboration with the European Space Agency's solar orbiter [1][2] Group 1 - The Parker Solar Probe, launched in 2018, is the only spacecraft capable of entering the solar upper atmosphere for direct measurements [1] - The probe captured a significant solar eruption on September 6, 2022, allowing for high-resolution imaging and sampling of plasma and magnetic field characteristics [1] - This breakthrough enables scientists to better understand the mechanisms of solar energy transfer and particle acceleration, improving the accuracy of solar activity predictions [2]

Core Insights - The research team from the Yunnan Astronomical Observatory has revealed the physical mechanism of oscillatory magnetic reconnection in the solar atmosphere, providing a new theoretical model for understanding the periodic variations of solar activities such as solar flares and coronal mass ejections [1][2] Group 1: Research Findings - The study utilized 2.5D radiative magnetohydrodynamic simulations to reconstruct the process of magnetic flux ropes rising from the convection zone to the atmosphere and reconnecting with the background magnetic field [1] - The simulations indicated that the direction of the current sheet exhibits quasi-periodic reversals, with reversal periods concentrated between 8 to 15 minutes, and the longest reaching 30 minutes, aligning closely with observational data [1] - The research identified that the convection and turbulence in the solar convection zone are key drivers of the oscillatory behavior of magnetic reconnection [2] Group 2: Implications for Solar Activity - The study proposes a new mechanism for oscillatory magnetic reconnection by coupling the dynamics of the convection zone with coronal magnetic reconnection, addressing previous discrepancies between simulation periods and observations [2] - The periodic fluctuations in the magnetic reconnection rate, ranging from 100 to 400 seconds, correlate with the oscillation periods of solar acoustic waves, suggesting a deep connection between internal solar motions and atmospheric activities [2] - This research enhances the understanding of solar activity's periodic pulsations, which could lead to more accurate predictions of solar storms' impacts on Earth [2]

Core Insights - The TRACERS mission aims to study magnetic reconnection around Earth to understand how the Sun interacts with Earth's protective magnetic shield, the magnetosphere [2] Group 1 - The mission focuses on the interaction between solar activity and Earth's magnetosphere [2] - TRACERS will provide insights into the mechanisms of magnetic reconnection [2] - Understanding these interactions is crucial for comprehending space weather impacts on Earth [2]