The magnetic and convective nature of the Sun’s photosphere provides a unique platform from which generated waves can be modelled, observed and interpreted across a wide breadth of spatial and temporal scales. As oscillations are generated in-situ or emerge through the photospheric layers, the interplay between the rapidly evolving densities, temperatures and magnetic field strengths provides dynamic evolution of the embedded wave modes as they propagate into the tenuous solar chromosphere. A focused science team was assembled to discuss the current challenges faced in wave studies in the lower solar atmosphere, including those related to spectropolarimetry and radiative transfer in the optically thick regions. Following the Theo Murphy international scientific meeting held at Chicheley Hall during February 2020, the scientific team worked collaboratively to produce 15 independent publications for the current Special Issue, which are introduced here. Implications from the current research efforts are discussed in terms of upcoming next-generation observing and high-performance computing facilities. This article is part of the Theo Murphy meeting issue ‘High-resolution wave dynamics in the lower solar atmosphere’.

中文翻译：

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太阳低层大气中的高分辨率波动力学


太阳光球层的磁性和对流性质提供了一个独特的平台，可以在广泛的空间和时间尺度上对所产生的波进行建模、观察和解释。当振荡在原位产生或通过光球层出现时，快速变化的密度、温度和磁场强度之间的相互作用提供了嵌入波模式在传播到脆弱的太阳色球层时的动态演化。组建了一个重点科学团队，讨论当前太阳大气层低层波动研究面临的挑战，包括与分光偏振法和光学厚区域辐射传输相关的挑战。继 2020 年 2 月在 Chicheley Hall 举行 Theo Murphy 国际科学会议之后，科学团队通力合作，为本期特刊制作了 15 篇独立出版物，在此介绍。讨论了当前研究工作对即将推出的下一代观测和高性能计算设施的影响。本文是 Theo Murphy 会议问题“低层太阳大气中的高分辨率波动力学”的一部分。