Genesis and impulsive evolution of the 2017 September 10 coronal mass ejection
Astrid M. Veronig, Tatiana Podladchikova, Karin Dissauer, Manuela Temmer, Daniel B. Seaton, David Long, Jingnan Guo, Bojan Vrsnak, Louise Harra, Bernhard Kliem
2017年9月10日的X8.2事件提供了独特的观测，以研究非常快速的CME的成因，磁性形态和脉冲动力学。结合GOES-16/SUVI和SDO/AIA EUV图像，我们确定了一个热（$T\approx 10-15$ MK）明亮的边缘周围的快速膨胀的空腔，嵌入一个更大的CME壳（$T\approx 1-2$ MK）。CME壳层由一组密集的大AR环（$\gtrsim$ 0.5 $R_s$）发展而来，并无缝地演变成LASCO C2观测到的CME锋面。CME壳层强烈的横向过度膨胀就像一个活塞，启动了快速的EUV波。热腔边缘被证明是一种表现的主导极向通量和冻结的等离子体添加到上升的通量绳的磁重联在电流片下面。同样的结构后来被观察到作为白光CME的核心，挑战了CME三部分形态的传统解释。这些观测结果所建议的大量增加的磁通量解释了CME壳和腔的径向和横向膨胀的极端加速度，所有这些加速度都达到了$5 - 10$ km s $^{-2}$的值。加速峰值同时发生的第一RHESSI $100-300$ keV的硬X射线爆发的相关耀斑，进一步强调的重要性，脉冲CME演变的重联过程。最后，磁通绳相对于CME壳层的更高的径向传播速度导致白光CME波前和激波的明显变形。
英文摘要：
The X8.2 event of 10 September 2017 provides unique observations to study the genesis, magnetic morphology and impulsive dynamics of a very fast CME. Combining GOES-16/SUVI and SDO/AIA EUV imagery, we identify a hot ($T\approx 10-15$ MK) bright rim around a quickly expanding cavity, embedded inside a much larger CME shell ($T\approx 1-2$ MK). The CME shell develops from a dense set of large AR loops ($\gtrsim$0.5 $R_s$), and seamlessly evolves into the CME front observed in LASCO C2. The strong lateral overexpansion of the CME shell acts as a piston initiating the fast EUV wave. The hot cavity rim is demonstrated to be a manifestation of the dominantly poloidal flux and frozen-in plasma added to the rising flux rope by magnetic reconnection in the current sheet beneath. The same structure is later observed as the core of the white light CME, challenging the traditional interpretation of the CME three-part morphology. The large amount of added magnetic flux suggested by these observations explains the extreme accelerations of the radial and lateral expansion of the CME shell and cavity, all reaching values of $5 - 10$ km s$^{-2}$. The acceleration peaks occur simultaneously with the first RHESSI $100-300$ keV hard X-ray burst of the associated flare, further underlining the importance of the reconnection process for the impulsive CME evolution. Finally, the much higher radial propagation speed of the flux rope in relation to the CME shell causes a distinct deformation of the white light CME front and shock.
Heating of a plasma sheet in nonequilibrium ionization with nonthermal electrons
Kyung Hee University（庆熙大学）；Yunnan Observatories, Chinese Academy of Sciences（中国科学院云南天文台）；Air Force Research Laboratory（美国空军研究实验室）；G-LAMP NEXUS Institute/School of Space Research, Kyung Hee University（庆熙大学G-LAMP NEXUS研究所/空间研究学院）；Korea Astronomy & Space Science Institute（韩国天文学与空间科学研究院）
Elemental Composition Evolution during the 2024 September 30 Solar Eruption: A Comparison of Hot and Cool Plasma Components with Solar Orbiter/SPICE, Hinode/EIS, and Chandrayaan-2/XSM
Southwest Research Institute（西南研究所）；Ann and H.J. Smead Aerospace Engineering Sciences, University of Colorado Boulder（科罗拉多大学博尔德分校安与H.J.斯梅德航空航天工程科学系）；Laboratory for Atmospheric and Space Physics, University of Colorado Boulder（科罗拉多大学博尔德分校大气与空间物理实验室）；University of Alabama in Huntsville（阿拉巴马大学亨茨维尔分校）；NASA Marshall Space Flight Center（美国国家航空航天局马歇尔太空飞行中心）
