There have been ubiquitous observations of wave-like motions in the solar atmosphere for decades. Recent improvements to space- and ground-based observatories have allowed the focus to shift to smaller magnetic structures on the solar surface. In this paper, high-resolution ground-based data taken using the Swedish 1 m Solar Telescope is combined with co-spatial and co-temporal data from the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory (SDO) satellite to analyze running penumbral waves (RPWs). RPWs have always been thought to be radial wave propagation that occurs within sunspots. Recent research has suggested that they are in fact upwardly propagating field-aligned waves (UPWs). Here, RPWs within a solar pore are observed for the first time and are interpreted as UPWs due to the lack of a penumbra that is required to support RPWs. These UPWs are also observed co-spatially and co-temporally within several SDO/AIA elemental lines that sample the transition region and low corona. The observed UPWs are traveling at a horizontal velocity of around 17 ± 0.5 km s–1 and a minimum vertical velocity of 42 ± 21 km s–1. The estimated energy of the waves is around 150 W m–2, which is on the lower bound required to heat the quiet-Sun corona. This is a new, yet unconsidered source of wave energy within the solar chromosphere and low corona.
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机译：数十年来，在太阳大气中普遍观察到波浪状运动。对天基和地基天文台的最新改进已使焦点转移到了太阳表面的较小磁性结构上。在本文中，使用瑞典1 m太阳望远镜获得的高分辨率地面数据与太阳动力学天文台（SDO）卫星上大气成像组件（AIA）的同时和同时数据相结合，以进行分析运行半影波（RPW）。 RPW一直被认为是在黑子内发生的径向波传播。最近的研究表明，它们实际上是向上传播的场取向波（UPW）。在这里，首次观察到太阳孔隙内的RPW，由于缺乏支撑RPW的半影，因此被解释为UPW。这些UPW在几个SDO / AIA元素线中也同时在空间上和时间上被观测到，这些元素线对过渡区域和低电晕进行采样。观察到的UPW以大约17±0.5 km s-1的水平速度和最小42±21 km s-1的垂直速度行进。估计的波能量约为150 W m–2，处于加热安静的太阳日冕所需的下限。这是太阳色球层和低日冕中一种新的但尚未考虑的波能来源。
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