2024年9月30日太阳爆发期间的元素组成演化：利用Solar Orbiter/SPICE、Hinode/EIS和Chandrayaan-2/XSM对高温与低温等离子体成分的比较
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
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中文总结 AI 辅助
该研究利用Solar Orbiter、Hinode、Chandrayaan-2的相关仪器，观测2024年9月30日M7.6级太阳耀斑，发现高低温等离子体成分丰度演化模式不同，揭示了FIP偏差变化与日冕重联外流和色球层等离子体混合相关的机制。
中文摘要 AI 辅助
太阳等离子体的组成在不同时间尺度上存在光球层与日冕层之间的差异，具有低第一电离势（FIP）元素的优先增强现象。然而，FIP分馏的物理起源尚未完全明确。此外，在耀斑期间，FIP偏差也会出现快速变化，这与不同FIP偏差物质的快速传输相关。我们展示了来自Solar Orbiter SPICE和EUI、Hinode/EIS以及Chandrayaan-2 XSM仪器的新观测结果，发现在2024年9月30日观测到的M7.6级爆发性太阳耀斑期间，发射等离子体的丰度在数分钟的时间尺度上发生了快速变化。这些仪器具有宽广的温度覆盖范围，发现高温与低温等离子体成分之间存在截然不同的丰度演化模式。对活动区的三维重建以及Solar Orbiter STIX X射线望远镜的额外观测表明，不同仪器在不同光谱区域观测到的高温与低温等离子体成分，采样了所观测耀斑等离子体不同位置的等离子体组成演化。SPICE观测到的明亮耀斑后环顶显示出日冕FIP偏差，而XSM观测到的高温等离子体在脉冲阶段FIP偏差从日冕向光球层降低。我们将这些观测结果解释为X射线诊断观测到的高温日冕重联外流与色球层等离子体混合的证据，随着耀斑环依次被激活和松弛，解释了FIP偏差为何从日冕向混合态降低；而SPICE观测到的低温环顶因日冕物质沉积在环顶附近而显示出日冕丰度。
英文摘要
Solar plasma composition differs between the photosphere and corona over a range of timescales, with preferential enhancement of elements with low first ionization potential (FIP). However, the physical origin of the FIP fractionation remains incompletely understood. Furthermore, during flares, the FIP bias also exhibits rapid changes, associated with fast transport of material with different FIP biases. We present novel observations from Solar Orbiter SPICE and EUI, Hinode/EIS, and Chandrayaan-2 XSM instruments, finding rapid abundance changes in the emitting plasma, on timescales of minutes, during the eruptive M7.6-class solar flare observed on 2024 Sept 30. These instruments have wide temperature coverage and find contrasting abundance-evolution patterns between the hotter and cooler plasma components. 3D reconstruction of the active region and additional observations from the Solar Orbiter STIX X-ray telescope show how the hot and cool plasma components, emitting in different spectral regions and observed with the various instruments, sample the plasma composition evolution in distinct locations within the observed flaring plasma. The bright post-flare loop tops observed by SPICE show coronal FIP bias, while the hot plasma observed with XSM exhibits FIP-bias decreasing from coronal to photospheric during the impulsive phase. We interpret these observations as evidence of the X-ray diagnostics seeing hot coronal reconnection outflows mixing with chromospheric plasma as flare loops sequentially energize and relax, explaining why the FIP bias decreases from coronal to a hybrid; and the cool loop tops seen with SPICE show coronal abundances due to coronal material deposited near the looptops.
