发表机构
Laboratory for Atmospheric and Space Physics, University of Colorado Boulder; Southwest Research Institute; Department of Physics and Astronomy, University of Florence; Climate and Space Sciences and Engineering, University of Michigan; Physics Department, University of California, Berkeley; Space Sciences Laboratory, University of California, Berkeley; The Blackett Laboratory, Imperial College London; Mullard Space Science Laboratory, University College London; Department of Physics and Astronomy, University of Iowa; University of Cambridge; University of Leicester; Space Exploration Sector, Johns Hopkins Applied Physics Laboratory; Johns Hopkins Applied Physics Laboratory; School of Engineering, Physics and Mathematics, Northumbria University; ESTEC, ESA; Predictive Science Inc.; Imperial College London（科罗拉多大学博尔德分校大气与空间物理实验室; 西南研究所; 佛罗伦萨大学物理与天文系; 密歇根大学气候与空间科学与工程; 加州大学伯克利分校物理系; 加州大学伯克利分校空间科学实验室; 帝国理工学院布莱克特实验室; 伦敦大学学院穆拉德空间科学实验室; 爱荷华大学物理与天文系; 剑桥大学; 莱斯特大学; 约翰斯·霍普金斯大学应用物理实验室太空探索部; 约翰斯·霍普金斯大学应用物理实验室; 诺森比亚大学工程、物理与数学学院; 欧洲空间局欧洲空间研究与技术中心; 预测科学公司; 帝国理工学院）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究利用多视角遥感与原位测量，计算了日冕洞太阳风从低日冕到日球层的能量收支，发现压缩磁流体力学波能通量对维持能量平衡至关重要，且能量主要在阿尔芬表面内转化为离子加热与加速。
AI 中文摘要
利用协调的地基和天基遥感观测，提供了太阳大气的全面、多视角视图，并将其与围绕2024年4月8日在北美观测到的日全食的日球层原位测量联系起来。这些近同时的多波长数据集被用于直接推导等离子体参数，并计算太阳风流在其低日冕诞生地（高度为1.05太阳半径）的能量收支。同一太阳风流的能量收支也通过原位观测在阿尔芬表面及其之外独立计算。总波能通量主导低日冕收支（阿尔芬波为11瓦每平方米，压缩磁流体力学模式为7至23瓦每平方米），而焓（13瓦每平方米）和从1.0太阳半径克服重力所做的功（2.5瓦每平方米）构成其余部分。当且仅当包含压缩能通量并将其归因于快磁声波模式时，总日冕能量收支与帕克太阳探测器实测的总能量收支一致。几乎所有这种热能和波能都在阿尔芬表面内转化为离子加热、加速和重力势能。该太阳风流的演化很好地描述为热压驱动的风，并伴有磁流体力学波动沉积的额外能量。这些波动的阿尔芬分量观测到的演化在阿尔芬表面以下遵循近乎无耗散的曲线，而在该临界表面以上则更强烈地偏离该曲线。
英文摘要
Coordinated ground- and space-based remote observations are used to provide a comprehensive, multi-perspective view of the solar atmosphere that we connect with in situ measurements in the heliosphere centered around the April 8 2024 Total Solar Eclipse observed across North America. These near-contemporaneous, multi-wavelength datasets are used to directly derive the plasma parameters and compute an energy budget of a solar wind stream at its low-coronal birthplace (at an altitude of 1.05Rsun). The energy budget is also independently computed at and beyond the Alfvén surface from the in situ observations of the same stream. The total wave energy flux dominates the low-coronal budget (11 W m-2 Alfvén, 7 to 23 W m-2 in compressive MHD modes), while enthalpy (13 W m-2) and work done against gravity from 1.0Rsun (2.5 W m-2) make up the remainder. The total coronal energy budget is consistent with the total measured in situ by Parker Solar Probe if and only if compressive energy flux is included and attributed to the fast magnetosonic mode. Nearly all this thermal and wave energy is converted to ion heating, acceleration and gravitational potential energy within the Alfvén surface. The stream evolution is well-described as a thermal-pressure driven wind with additional energy deposited by MHD fluctuations. The observed evolution of the Alfvénic component of these fluctuations follows a near-dissipation-free curve below the Alfvén surface while deviating from it more strongly above this critical surface.
CommentsThe manuscript has been accepted to ApJ
