The significance increase of the plasma temperature from the solar photosphere to the corona up to 1MK is still unresolved. One of the candidates for this issue is waves and instabilities in the solar plasma. It was suggested that the energy of these waves could heat the solar atmosphere to transition-region (TR) and corona. Despite many recent kind of researches about waves in the various solar dynamic structures, the reasons for the sudden rise of solar atmospheric temperature are still not enough. By using the Interface Region Imaging Spectrograph (IRIS) telescope observations, we investigate the waves in magnetic tubes such as UV bright points (BPs) at the boundary and inside the supper-granules. The Study of these dynamic structures, between the chromosphere and transition region, will impressively increase our information of mass and energy transportation through interface region between the chromosphere and inner corona. The magnetic BPs are the faces of magnetic flux tubes that are associated with magnetic elements. The magnetic flux tubes expand upward and appear as bright grains that make up the chromospheric network. For investigating periodical behavior of these structures and various aspect of these oscillations, we analyze intensity oscillations individually in IRIS slit-jaw images at three filters included 2796 Å, 1400 Å and 1330 Å by the wavelet analysis method. The wavelet analysis of the intensity fluctuations of these points showed periods from 2 to 8 min, which are in order of the frequencies of the atmospheric pressure modes. For investigating wave propagation in these layers we also study the correlation of oscillations between chromosphere (2796 Å) and TR (1400 Å and 1330 Å) heights by cross wavelet method, and found that these heights correlate with periods between 2.5 and 5.5 min, with wave speeds from 30 to 200 km s −1 . Also, by extracting Si IV line, we determined the Doppler velocity of BPs in the network and inter-network as about −20 to +30 km s −1 and −21 to +21 km s −1 , respectively. Our results suggest that the wave propagation along the magnetic flux tubes of upward-moving plasma in BPs have an important role in solar atmosphere heating.

中文翻译：

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波在色球层和过渡区域之间的网络和网络间亮点通道中的传播与 IRIS 观测

从太阳光球到日冕的等离子体温度显着增加高达 1MK 的问题仍未解决。这个问题的候选者之一是太阳等离子体中的波和不稳定性。有人提出，这些波的能量可以将太阳大气加热到过渡区（TR）和日冕。尽管最近对各种太阳动力结构中的波进行了大量研究，但对太阳大气温度突然升高的原因仍然不够。通过使用界面区域成像光谱仪 (IRIS) 望远镜观测，我们研究了磁管中的波，例如边界和超颗粒内部的紫外线亮点 (BP)。这些动态结构的研究，在色球和过渡区域之间，将通过色球层和内日冕之间的界面区域显着增加我们的质量和能量传输信息。磁性 BP 是与磁性元件相关联的磁通量管的表面。磁通管向上扩展并显示为构成色球网络的明亮颗粒。为了研究这些结构的周期性行为和这些振荡的各个方面，我们通过小波分析方法在包括 2796 Å、1400 Å 和 1330 Å 的三个滤波器上分别分析了 IRIS 裂口图像中的强度振荡。这些点的强度波动的小波分析显示周期为 2 到 8 分钟，按大气压力模式的频率顺序排列。为了研究这些层中的波传播，我们还通过交叉小波方法研究了色球（2796 Å）和 TR（1400 Å 和 1330 Å）高度之间振荡的相关性，发现这些高度与 2.5 到 5.5 分钟之间的周期相关，与波速从 30 到 200 km s -1 。此外，通过提取 Si IV 线，我们确定网络和网络间 BP 的多普勒速度分别约为 -20 至 +30 km s -1 和 -21 至 +21 km s -1 。我们的研究结果表明，波在 BPs 中沿向上运动等离子体的磁通量管传播在太阳大气加热中具有重要作用。波速从 30 到 200 km s -1 。此外，通过提取 Si IV 线，我们确定网络和网络间 BP 的多普勒速度分别约为 -20 至 +30 km s -1 和 -21 至 +21 km s -1 。我们的研究结果表明，波在 BPs 中沿向上运动等离子体的磁通量管传播在太阳大气加热中具有重要作用。波速从 30 到 200 km s -1 。此外，通过提取 Si IV 线，我们确定网络和网络间 BP 的多普勒速度分别约为 -20 至 +30 km s -1 和 -21 至 +21 km s -1 。我们的研究结果表明，波在 BPs 中沿向上运动等离子体的磁通量管传播在太阳大气加热中具有重要作用。