THE DETECTION OF UPWARDLY PROPAGATING WAVES CHANNELING ENERGY FROM THE CHROMOSPHERE TO THE LOW CORONA
THE DETECTION OF UPWARDLY PROPAGATING WAVES CHANNELING ENERGY FROM THE CHROMOSPHERE TO THE LOW CORONA
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DOI：
10.1088/0004-637x/791/1/61
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发表时间：
2014-07
期刊：
影响因子：
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通讯作者：
N. Freij;E. Scullion;E. Scullion;C. J. Nelson;C. J. Nelson;Stuart Mumford;S. Wedemeyer;R. Erdélyi
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文献类型：
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作者：
N. Freij;E. Scullion;E. Scullion;C. J. Nelson;C. J. Nelson;Stuart Mumford;S. Wedemeyer;R. Erdélyi
几十年来，人们对太阳大气中的波动运动进行了普遍的观测。最近对空间和地面观测站的改进使重点转向太阳表面较小的磁结构。在本文中，高分辨率的地面数据，使用瑞典1米太阳望远镜的空间和时间的数据相结合的大气成像组件（AIA）的太阳动力学观测（SDO）卫星上分析运行半影波（RPWs）。RPW一直被认为是发生在太阳黑子内的径向波传播。最近的研究表明，它们实际上是向上传播的场向波（UPWs）。在这里，RPWs在太阳能孔内首次被观察到，并被解释为UPWs由于缺乏半影，需要支持RPWs。这些UPW也被观察到co-spatially和co-temporarily内的几个SDO/AIA元素线，采样的过渡区和低电晕。观测到的UPW的水平速度约为17 ± 0.5 km s−1，最小垂直速度为42 ± 21 km s−1。波的估计能量约为150 W m−2，这是加热平静日冕所需的下限。这是太阳色球层和低日冕中一种新的、尚未被考虑的波能来源。
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.