寻找磁性亮点中的模式耦合

Arthur Berberyan, Peter H. Keys, David B. Jess, Damian J. Christian
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摘要

背景。磁亮点(MBPs)是太阳大气中磁场的最小表现形式之一,据观测可从光球层一直延伸到色球层。因此,在太阳大气中寻找磁流体动力(MHD)波和模式耦合类型时,它们是一个极好的特征。在这项工作中,我们旨在通过寻找可能的模式耦合来比较光球和色球层的强度振荡,从而研究波在太阳低层大气中的传播,以确定这些类型的波在太阳大气中的重要性,以及它们对加热色球层的贡献。方法:2011 年 7 月,利用邓恩太阳望远镜的 ROSA 和 HARDCaminstruments 进行了观测。我们使用小波分析来识别移动的MHD波,并得出G波段和H$\alpha$波段的频率。在整个观测过程中,我们使用一种自动跟踪算法分离出了大量的MBPs样本。从样本中挑选出二十几个最亮的 MBPs 进行进一步研究。结果。我们在 G 波段的 MBPs 中发现了振荡,频率在 1.5 到 3.6 mHz 之间。用 H$\alpha$ 观测到的低层日光层中的相应 MBP 的频率范围为 1.4 到 4.3 mHz。在大约 38%的 MBPs 中,H$\alpha$ 与 G 波段频率之比接近 2。因此,这些振荡显示了一种模式耦合形式,即光球中的横波被转换成色球中的纵波。结论通过简单的估算,我们发现能量通量大约为 45 $\times 10^{3}$ W m$^{-2}$,并表明流经MBPs的能量足以加热色球层,而模式耦合对于帮助我们理解太阳低层大气中的MHD波类型和整体能量预算非常重要。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
A search for mode coupling in magnetic bright points
Context. Magnetic bright points (MBPs) are one of the smallest manifestations of the magnetic field in the solar atmosphere and are observed to extend from the photosphere up to the chromosphere. As such, they represent an excellent feature to use in searches for types of magnetohydrodynamic (MHD) waves and mode coupling in the solar atmosphere. Aims. In this work, we aim to study wave propagation in the lower solar atmosphere by comparing intensity oscillations in the photosphere with the chromosphere via a search for possible mode coupling, in order to establish the importance of these types of waves in the solar atmosphere, and their contribution to heating the chromosphere. Methods. Observations were conducted in July 2011 with the ROSA and the HARDCam instruments at the Dunn Solar Telescope. We used wavelet analysis to identify traveling MHD waves and derive frequencies in the G-band and H$\alpha$wave bands. We isolated a large sample of MBPs using an automated tracking algorithm throughout our observations. Two dozen of the brightest MBPs were selected from the sample for further study. Results. We find oscillations in the G-band MBPs, with frequencies between 1.5 and 3.6 mHz. Corresponding MBPs in the lower solar chromosphere observed in H$\alpha$ show a frequency range of 1.4 to 4.3 mHz. In about 38\% of the MBPs, the ratio of H$\alpha$ to G-band frequencies was near two. Thus, these oscillations show a form of mode coupling where the transverse waves in the photosphere are converted into longitudinal waves in the chromosphere. Conclusions. From simple estimates we find an energy flux of $\approx$45 $\times 10^{3}$ W m$^{-2}$ and show that the energy flowing through MBPs is enough to heat the chromosphere, and mode coupling is important in helping us understand the types of MHD waves in the lower solar atmosphere and the overall energy budget.
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