Connectivity between the solar photosphere and chromosphere in a vortical structure. Observations of multi-phase, small-scale magnetic field amplification

S. M. Díaz-Castillo, C. E. Fischer, R. Rezaei, O. Steiner, S. Berdyugina
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Abstract

High-resolution solar observations have revealed the existence of small-scale vortices, as seen in chromospheric intensity maps and velocity diagnostics. Frequently, these vortices have been observed near magnetic flux concentrations, indicating a link between swirls and the evolution of the small-scale magnetic fields. Vortices have also been studied with magneto-hydrodynamic (MHD) numerical simulations of the solar atmosphere, revealing their complexity, dynamics, and magnetic nature. In particular, it has been proposed that a rotating magnetic field structure driven by a photospheric vortex flow at its footprint produces the chromospheric swirling plasma motion. We present a complete and comprehensive description of the time evolution of a small-scale magnetic flux concentration interacting with the intergranular vortex flow and affected by processes of intensification and weakening of its magnetic field. In addition, we study the chromospheric dynamics associated with the interaction, including the analysis of a chromospheric swirl and an impulsive chromospheric jet.
涡旋结构中太阳光层和色球层之间的联系。多相小尺度磁场放大观测
高分辨率太阳观测揭示了小尺度漩涡的存在,正如在色球强度图和速度诊断中看到的那样,这些漩涡经常在磁通量集中附近被观测到,表明漩涡与小尺度磁场的演变之间存在联系。我们还利用太阳大气的磁流体动力(MHD)数值模拟对漩涡进行了研究,揭示了它们的复杂性、动力学和磁性。特别是,有人提出,由光球漩涡流驱动的旋转磁场结构在其足迹处产生了色球层漩涡等离子体运动。我们完整而全面地描述了与晶间漩涡流相互作用并受其磁场增强和减弱过程影响的小尺度磁通量浓度的时间演变。此外,我们还研究了与相互作用相关的色球层动力学,包括分析非色球层漩涡和脉冲色球层射流。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
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