通量绳俘获的微型日珥爆发及耀斑后日冕雨的多波长合成研究
Multi-wavelength synthesis of a flux rope-trapped mini-prominence eruption and post-flare coronal rain
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中文总结 AI 辅助
该研究通过2.5维MHD模拟结合多波长合成诊断，揭示了太阳上通量绳俘获的微型日珥爆发及耀斑后日冕雨的多热结构，为相关高分辨率观测提供了特征指引。
中文摘要 AI 辅助
尽管高分辨率观测不断增加，但太阳日冕中的小规模爆发现象，包括微型通量绳及相关的冷等离子体凝聚体，仍未被完全理解。我们基于2.5维磁流体力学（MHD）模拟开展正向建模，该模拟捕捉了同源通量绳爆发、原位凝聚形成微型日珥以及后续耀斑后日冕雨的过程。通过光学薄的极紫外（EUV）和紫外（UV）辐射，以及针对Hα线的非局部热动平衡（non-LTE）辐射转移处理，获得了合成诊断结果。合成EUV辐射显示通量绳呈现明亮的边缘状结构；对应的UV诊断显示明亮区域，该区域与通量绳内部因嵌入冷等离子体（约数万开）形成的暗核共空间，从而识别出正在爆发的微型日珥。Si IV 1402.77埃的光谱合成表明微型纤维向上运动，并揭示爆发过程中存在两个主要速度分量。在后续阶段，耀斑后拱廊中的热不稳定性产生温度约为10^4开的日冕雨；EUV诊断显示雨团下游出现增亮，表明与压缩效应相关的局地加热。Hα光谱合成显示增强的吸收特征和红移轮廓，对应日冕雨团的下落速度可达约23千米每秒，而Si IV 1402.77埃光谱轮廓显示最大下落速度约为50千米每秒，突出了下落雨团内部热力学和运动学结构的证据。合成诊断提供了清晰的多波长特征，可指导未来的高分辨率观测，并强调了小规模重联驱动过程在塑造太阳日冕多热结构（从兆开到数千开）中的重要性。
英文摘要
Small-scale eruptive phenomena in the solar corona including miniature flux ropes and associated cool plasma condensations are not fully understood despite increasing high-resolution observations. We perform forward modeling based on a 2.5D MHD simulation capturing homologous flux rope eruptions, in-situ condensation leading to a mini-prominence, and subsequent post-flare coronal rain. Synthetic diagnostics are obtained using optically-thin EUV and UV emissions, and non-LTE radiative transfer treatment for the H$α$ line. The synthetic EUV emission reveals the flux ropes as bright rim-like structures. The corresponding UV diagnostic shows bright region, which is co-spatial with the dark core due to embedded cool plasma ($\sim$ tens of kK) inside the flux rope, identifying an erupting mini-prominence. Spectral synthesis of Si IV 1402.77 A indicates an upward motion of the mini-filament, and reveals the presence of two predominant velocity components during eruption. At a later stage, thermal instability in post-flare arcades produces coronal rain with temperatures of $\approx 10^4$ K. The EUV diagnostics reveal brightening at the downstream of the rain blob, indicating localized heating associated with compressional effects. The H$α$ spectral synthesis shows enhanced absorption signatures and red-shifted profiles corresponding to downflows of the coronal rain blobs up to $\approx 23$ km s$^{-1}$, whereas the Si IV 1402.77 A spectral profile shows the maximum downflow velocity of $\approx50$ km s$^{-1}$, highlighting the evidence of thermodynamic and kinematic structuring within the falling rain blobs. The synthetic diagnostics provide clear, multi-wavelength signatures that can guide future high-resolution observations, and highlight the importance of small-scale reconnection-driven processes in shaping the multi-thermal structure (between MK to kK) of the solar corona.
发表机构
- Instituto de Astrofísica de Canarias（加那利天体物理研究所）
- Universidad de La Laguna（拉古纳大学）
- University of Helsinki（赫尔辛基大学）
- Leibniz-Institut für Astrophysik Potsdam (AIP)（波茨坦莱布尼茨天体物理研究所）
- NASA Goddard Space Flight Center（美国宇航局戈达德太空飞行中心）
- Northumbria University（诺森比亚大学）
机构由 AI 辅助整理，请以论文原文为准。
