发表机构
Max-Planck-Institut für Sonnensystemforschung; Grupo de Estudios en Heliofísica de Mendoza, CONICET, Universidad de Mendoza; Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences（马克斯·普朗克太阳系统研究所; 门多萨日物理研究组，阿根廷国家科学研究委员会，门多萨大学; 暗物质和空间天文重点实验室，中国科学院紫金山天文台）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
通过SUNRISE天文台的高分辨率观测发现，太阳耀斑色球层深处约100 km尺度的小尺度蒸发流早于非热电子出现，为研究耀斑低层大气加热与质量循环提供了新视角，挑战了标准太阳耀斑模型。
AI 中文摘要
耀斑由太阳大气中磁能的突然释放引发，填充耀斑后日冕的温度远超10 MK的等离子体源于较冷色球层物质的快速加热与消融，这种色球蒸发被认为主要由撞击低层大气的非热电子促成。然而，这些上行流在色球层中何时、何处产生的问题尚未完全解决。本文报告了由气球载SUNRISE天文台搭载的SUNRISE紫外光谱偏振仪和成像仪记录的M级耀斑的前所未有的高分辨率观测结果，这些观测揭示了起源于色球层深处、空间尺度约100 km的高度结构化上行流。这些流甚至比非热电子的出现早约10分钟，且持续至耀斑的脉冲相。我们的观测为耀斑中低层大气加热和质量循环提供了新的认识，这些认识难以与标准太阳耀斑模型相调和。
英文摘要
Flares are caused by an abrupt release of magnetic energy in the solar atmosphere. Plasma heated to well over 10 MK filling the post-flare corona originates from a rapid heating and ablation of the cooler chromospheric material. This chromospheric evaporation is thought to be facilitated primarily by nonthermal electrons impinging on to the lower atmosphere. Questions on when and where in the chromosphere these upflows originate, however, are not fully resolved. Here we report on unprecedented high-resolution observations of an M-class flare recorded by the Sunrise Ultraviolet Spectropolarimeter and Imager on board the balloon-borne SUNRISE observatory, that reveal highly structured upflows on spatial scales of ~100 km originating deep in the chromosphere. The flows even precede the onset of nonthermal electrons by about 10 minutes and last through the impulsive phase of the flare. Our observations shed new light on the lower atmospheric heating and mass circulation in flares that are challenging to reconcile with the standard solar flare model.
CommentsPublished in the Astrophysical Journal Letters (Issue: Sunrise III Early Science)
Journal refApJL 1008 L65 (2026)
