发表机构
KU Leuven; NASA Goddard Space Flight Center; LPC2E, OSUC, Univ Orleans, CNRS, CNES（荷语鲁汶大学; 美国国家航空航天局戈达德太空飞行中心; 奥尔良大学、法国国家科学研究中心、法国国家航天研究中心）
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UAWSoM模块进行2.5维模拟，发现阿尔芬波不触发日冕凝聚体，而扭结波在精细结构半径约100公里时可触发形态独特的日冕雨，且两种波留下不同热力学特征。
AI 中文摘要
日珥和日冕雨是日冕凝聚体的两种表现形式，其形成机制目前仍仅被部分理解。尽管先前的研究已探索了局域化稳态或随机加热如何触发热不稳定性和凝聚体，但波驱动的能量输运和耗散的作用尚未得到广泛研究。在太阳大气中，阿尔芬波和扭结波是丰富的能量来源，能够同时贡献于日冕加热和等离子体结构形成，使其成为我们观测到的日冕结构形成过程中的有力候选者。我们旨在探索阿尔芬波和扭结波能量及其耗散如何影响日冕磁结构中凝聚体的形成和演化。特别是，我们独立于参数化的外部加热机制来研究每种波的作用，以隔离任一波动是否能触发凝聚体。我们使用开源MPI AMRVAC代码以及新开发的UAWSoM模块进行2.5维模拟。该模块自洽地演化阿尔芬波和扭结波能量及其通过波压和加热项对等离子体的反馈。我们检查了凝聚体形成的条件、其形态及其动力学演化。我们的结果表明，在我们的参数范围内，在2.5维磁流体动力学中，阿尔芬波未触发日珥或凝聚体的形成。我们发现，如果支撑扭结波的精细结构半径约为100公里，则扭结波可以触发日冕雨，其形态与由参数化加热函数触发的日冕雨有显著差异。通过使用UAWSoM，我们已确定在相同的波能量注入下，阿尔芬波和扭结波在日冕环上留下不同的热力学特征。
英文摘要
Prominences and coronal rain are two manifestations of coronal condensations whose formation mechanisms remain only partially understood. While previous studies have explored how localised steady or stochastic heating can trigger thermal instability and condensations, the role of wave driven energy transport and dissipation has not been extensively investigated. In the solar atmosphere, Alfven and kink waves are an abundant source of energy capable of contributing both to coronal heating and plasma structuring, making them compelling candidates in the formation processes of the structures we observe in the corona. We aim to explore how Alfven and kink wave energy and their dissipation influence the formation and evolution of condensations in coronal magnetic structures. In particular, we investigate each waves role independently of parameterised external heating mechanisms to isolate whether either wave can trigger condensations. We perform 2.5D simulations using the open source MPI AMRVAC code extended with the newly developed UAWSoM module. This module self consistently evolves Alfven and kink wave energy and their feedback on the plasma through wave pressure and heating terms. We examine the conditions under which condensations form, their morphology, and their dynamical evolution. Our results show that for our range of parameters, in 2.5D MHD, Alfven waves did not trigger the formation of prominences or condensations. We find that if the radius of the fine scale structures supporting the kink waves is of the order of 100 km, then kink waves can trigger coronal rain that differs considerably in its morphology from coronal rain triggered by parameterised heating functions. Through the use of UAWSoM, we have established that Alfven and kink waves leave distinct thermodynamic signatures on coronal loops, given the same wave energy injection.
Comments15 pages, 10 figures
