Vortex dynamics in various solar magnetic field configurations

IF 4.7 3区 物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS
Arjun Kannan, Nitin Yadav
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Abstract

We investigate vortex dynamics in three magnetic regions, viz., Quiet Sun, Weak Plage, and Strong Plage, using realistic three-dimensional simulations from a comprehensive radiation-magnetohydrodynamics (MHD) code, MURaM. We find that the spatial extents and spatial distribution of vortices vary for different set-ups even though the photospheric turbulence responsible for generating vortices has similar profiles for all three regions. We investigate kinetic and magnetic swirling strength and find them consistent with the Alfvén wave propagation. Using a flux tube expansion model and linear MHD wave theory, we find that the deviation in kinetic swirling strength from the theoretically expected value is the highest for the Strong Plage, least for the Weak Plage, and intermediate for the Quiet Sun at chromospheric heights. It suggests that Weak Plage is the most favoured region for chromospheric swirls, though they are of smaller spatial extents than in Quiet Sun. We also conjecture that vortex interactions within a single flux tube in Strong Plage lead to an energy cascade from larger to smaller vortices that further result in much lower values of kinetic swirling strength than other regions. Fourier spectra of horizontal magnetic fields at 1 Mm height also show the steep cascade from large to smaller scales for Strong Plage. These findings indicate the potential of vortex-induced torsional Alfvén waves to travel higher in the atmosphere without damping for weaker magnetic regions such as the Quiet Sun, whereas vortices would result in dissipation and heating due to the vortex interactions in narrow flux tubes for the strongly magnetized regions such as Strong Plage.
各种太阳磁场配置中的涡旋动力学
我们利用综合辐射-磁流体力学(MHD)代码 MURaM 进行了逼真的三维模拟,研究了三个磁区(即安静太阳、弱漩涡和强漩涡)的漩涡动力学。我们发现,尽管负责产生涡旋的光球层湍流在所有三个区域都具有相似的轮廓,但不同设置下涡旋的空间范围和空间分布却各不相同。我们研究了动漩涡和磁漩涡强度,发现它们与阿尔芬波传播相一致。利用通量管膨胀模型和线性 MHD 波理论,我们发现在色球高度上,强漩涡区的动漩涡强度与理论预期值的偏差最大,弱漩涡区最小,而静止太阳则介于两者之间。这表明弱漩涡是色球层漩涡的最有利区域,尽管其空间范围小于静止太阳。我们还推测,强漩涡区单个通量管内的漩涡相互作用导致能量从较大的漩涡级联到较小的漩涡,进一步导致动能漩涡强度值比其他区域低得多。1 毫米高度的水平磁场傅立叶频谱也显示了强漩涡从大尺度到小尺度的陡峭级联。这些发现表明,对于静止太阳等磁性较弱的区域,涡旋诱导的扭转阿尔弗韦恩波有可能在大气中传播得更高,而不会受到阻尼;而对于强磁化区域(如 Strong Plage),由于涡旋在狭窄磁通管中的相互作用,涡旋会导致耗散和加热。
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来源期刊
CiteScore
9.10
自引率
37.50%
发文量
3198
审稿时长
3 months
期刊介绍: Monthly Notices of the Royal Astronomical Society is one of the world''s leading primary research journals in astronomy and astrophysics, as well as one of the longest established. It publishes the results of original research in positional and dynamical astronomy, astrophysics, radio astronomy, cosmology, space research and the design of astronomical instruments.
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