In this work, a state-of-the-art vortex detection method, Instantaneous Vorticity Deviation, is applied to locate three-dimensional vortex tube boundaries in numerical simulations of solar photospheric magnetoconvection performed by the MURaM code. We detected three-dimensional vortices distributed along intergranular regions and displaying coned shapes that extend from the photosphere to the low chromosphere. Based on a well-defined vortex center and boundary, we were able to determine averaged radial profiles and thereby investigate the dynamics across the vortical flows at different height levels. The solar vortex tubes present nonuniform angular rotational velocity, and, at all height levels, there are eddy viscosity effects within the vortices, which slow down the plasma as it moves toward the center. The vortices impact the magnetic field as they help to intensify the magnetic field at the sinking points, and in turn, the magnetic field ends up playing an essential role in the vortex dynamics. The magnetic field was found to be especially important to the vorticity evolution. On the other hand, it is shown that, in general, kinematic vortices do not give rise to magnetic vortices unless their tangential velocities at different height levels are high enough to overcome the magnetic tension.

中文翻译：

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太阳涡流管：太阳大气中的涡流动力学

在这项工作中，在由 MURaM 代码执行的太阳光球层磁对流数值模拟中，应用了最先进的涡流检测方法瞬时涡度偏差来定位三维涡流管边界。我们检测到沿晶间区域分布的三维涡旋，并显示出从光球层延伸到低色球层的锥形形状。基于明确定义的涡流中心和边界，我们能够确定平均径向剖面，从而研究不同高度水平涡流的动力学。太阳涡流管呈现出不均匀的角旋转速度，并且在所有高度水平上，涡流内都存在涡粘性效应，这会在等离子体向中心移动时减慢其速度。涡流会影响磁场，因为它们有助于增强下沉点的磁场，反过来，磁场最终在涡流动力学中发挥重要作用。发现磁场对涡度演化特别重要。另一方面，研究表明，运动涡流通常不会产生磁涡流，除非它们在不同高度水平的切向速度足够高以克服磁张力。