论文标题
在太阳能轨道/EUI观察中具有明显能量的高频衰减波
High frequency decayless waves with significant energy in Solar Orbiter/EUI observations
论文作者
论文摘要
高频波现象引起了极大的兴趣，因为可能是为AC加热理论的一部分加热电晕所需的能量输入所需的能量输入。但是，直到太阳能轨道器使成像仪器的分辨率无法解决必要的时间和空间尺度。本文报道了位于电晕安静的太阳区域中的一个小环中的高频横向运动。使用EUI仪器的Hrieuv望远镜（17.4 nm）观察到振荡。我们在短循环中检测到两个横向振荡，长度为4.5毫米和11毫米。较短的回路显示为14 s的振荡，并且较长30 s。尽管有很高的分辨率，但没有确定的识别作为传播或站立波。对于较短且更长的回路，发现速度振幅分别等于72 km/s和125 km/s。基于此，我们还估计了回路中包含的能量通量的值 - 14 S振荡的能量为1.9 kW m^-2，而30 s振荡的振荡为6.5 kW m^-2。尽管在安静的阳光下观察到了这些振荡，但它们的能量通量与加热活性太阳能电晕所需的能量输入相同。进行数值模拟以重现观察到的振荡。数值结果对观测值的对应关系为观测值的能量含量估计提供了支持。在衰减的冠状波中尚未观察到这种高能量密度，这对于基于波浪阻尼的冠状加热模型是有希望的。
High-frequency wave phenomena present a great deal of interest as one of the possible candidates to contribute to the energy input required to heat the corona as a part of the AC heating theory. However, the resolution of imaging instruments up until the Solar Orbiter have made it impossible to resolve the necessary time and spatial scales. The present paper reports on high-frequency transverse motions in a small loop located in a quiet Sun region of the corona. The oscillations were observed with the HRIEUV telescope (17.4 nm) of the EUI instrument onboard the Solar Orbiter. We detect two transverse oscillations in short loops with lengths of 4.5 Mm and 11 Mm. The shorter loop displays an oscillation with a 14 s period and the longer a 30 s period. Despite the high resolution, no definitive identification as propagating or standing waves is possible. The velocity amplitudes are found to be equal to 72 km/s and 125 km/s, respectively, for the shorter and longer loop. Based on that, we also estimated the values of the energy flux contained in the loops - the energy flux of the 14 s oscillation is 1.9 kW m^-2 and of the 30 s oscillation it is 6.5 kW m^-2 . While these oscillations have been observed in the Quiet Sun, their energy fluxes are of the same order as the energy input required to heat the active solar corona. Numerical simulations were performed in order to reproduce the observed oscillations. The correspondence of the numerical results to the observations provide support to the energy content estimates for the observations. Such high energy densities have not yet been observed in decayless coronal waves, and this is promising for coronal heating models based on wave damping.
