论文标题
磁性线在模拟的太阳大气中扭曲
Magnetic thread twisting in a simulated solar atmosphere
论文作者
论文摘要
语境。血浆流入伴随太阳大气中的各种过程，例如加热冠状环和突出的形成。 目标。我们对分层的太阳大气进行了建模，其中模拟的突出线通过旨在模仿形成过程的血浆流入体验密度积累。我们旨在研究这种系统与扭转扰动的相互作用以及可能的后果。 方法。整合了运动和诱导的线性化方程，以分析在光球脚点随机驱动的扭转扰动的空间和时间演化。 结果。我们的结果表明，磁性线将经历扭曲放大。确定了不同的能量来源和水槽以及相应的扩增机制。达到色球高度的螺纹最容易受到磁性扭曲的影响，最大扭曲发生在其脚步附近。放大的曲折与沿模拟线程的常挥手行为相关联。 结论。我们的工作表明，扭转扰动可能会在突出线中放大，并且在脚上形成强磁曲折。放大过程在背景磁场中由小长度促进。另一方面，背景密度的长度尺寸很小会抑制生长。讨论了放大的曲折的可能后果，包括它们在支持突出结构内的密集血浆中的作用。
Context. Plasma inflows accompany a variety of processes in the solar atmosphere such as heating of coronal loops and formation of prominences. Aims. We model a stratified solar atmosphere, within which a simulated prominence thread experiences density accumulation via a plasma inflow designed to mimic the formation process. We aim to investigate the interaction of such a system with torsional perturbations, and the possible consequences. Methods. The linearised equations of motion and induction are integrated to analyse the spatial and temporal evolution of torsional perturbations that are randomly driven at the photospheric footpoints. Results. Our results demonstrate that magnetic threads will experience twist amplification. Different sources and sinks of energy and the corresponding amplification mechanisms are identified. Threads reaching chromospheric heights are most susceptible to magnetic twisting with the maximum twist occurring near their footpoints. The amplifying twists are associated with a standing wave behaviour along the simulated threads. Conclusions. Our work suggests that torsional perturbations may be amplified within prominence threads, with strong magnetic twists forming at the footpoints. The amplification process is facilitated by small length scales in the background magnetic field. On the other hand, a small length scale in the background density inhibits growth. Possible consequences of the amplified twists, including their role in supporting the dense plasma within a prominence structure are discussed.
