标题： 探索更热的日冕动态旋转轮廓：使用SDO/AIA数据的多波长方法 显示英文标题

标题： Exploring the dynamic rotational profile of the hotter solar atmosphere: A multi-wavelength approach using SDO/AIA data

摘要： 理解太阳大气的全球旋转轮廓及其变化是揭示太阳磁场动力学和不同太阳层之间耦合范围的关键。在本研究中，我们采用图像相关方法分析由太阳动力学观测台的大气成像组件在不同波长通道提供的大量数据。我们发现，在代表太阳大气的所有温度下，赤道旋转速率（$A$）显著增加，绝对纬度梯度（$|B|$）减少，这意味着赤道旋转速度可达$4.18\%$和$1.92\%$，比通过多普勒测量和黑子得出的底层光球的旋转速率更快，且差异更小。此外，我们在太阳大气的不同层还发现赤道旋转速率（$A$）显著增加，差异性（$|B|$减少）降低。 我们还探索了太阳内部到大气层的可能联系，并发现$A$在$r=0.94\,\mathrm{R}_{\odot}, 0.965\,\mathrm{R}_{\odot}$处分别与 171 埃、304 埃和 1600 埃有很好的匹配。 此外，我们观察到从 1600 埃、131 埃、193 埃和 211 埃测量的旋转参数与年平均黑子数之间存在正相关，这表明太阳旋转可能存在对与太阳周期相关的磁结构出现的依赖性，或者太阳大气中存在太阳旋转的周期依赖性。 显示英文摘要

摘要： Understanding the global rotational profile of the solar atmosphere and its variation is fundamental to uncovering a comprehensive understanding of the dynamics of the solar magnetic field and the extent of coupling between different layers of the Sun. In this study, we employ the method of image correlation to analyze the extensive dataset provided by the Atmospheric Imaging Assembly of the Solar Dynamic Observatory in different wavelength channels. We find a significant increase in the equatorial rotational rate ($A$) and a decrease in absolute latitudinal gradient ($|B|$) at all temperatures representative of the solar atmosphere, implying an equatorial rotation up to $4.18\%$ and $1.92\%$ faster and less differential when compared to the rotation rates for the underlying photosphere derived from Doppler measurement and sunspots respectively. In addition, we also find a significant increase in equatorial rotation rate ($A$) and a decrease in differential nature ($|B|$ decreases) at different layers of the solar atmosphere. We also explore a possible connection from the solar interior to the atmosphere and interestingly found that $A$ at $r=0.94\,\mathrm{R}_{\odot}, 0.965\,\mathrm{R}_{\odot}$ show an excellent match with 171 Angstrom, 304 Angstrom and 1600 Angstrom, respectively. Furthermore, we observe a positive correlation between the rotational parameters measured from 1600 Angstrom, 131 Angstrom, 193 Angstrom and 211 Angstrom with the yearly averaged sunspot number, suggesting a potential dependence of the solar rotation on the appearance of magnetic structures related to the solar cycle or the presence of cycle dependence of solar rotation in the solar atmosphere.