论文标题
冠状和太阳风在安静的阳光和冠状孔中：统一的情况
Coronal heating and solar wind formation in quiet Sun and coronal holes: a unified scenario
论文作者
论文摘要
在冠状通道中观察到冠状孔（CHS）比安静的太阳（QS）还黑。这项研究旨在使用\ ion {si} {4} 〜1394〜1394〜1394〜线在界面区域成像光谱仪（IRIS）录制的线路线（通过在Solar solar（HMI）上测量的磁场分布（SOD）在Solar Dynamils（Sdo）上，通过界面区域成像光谱仪（IRIS）来了解界面区域成像光谱仪（IRIS）记录的相似性和差异。我们发现，在CHS中获得的\ ion {si} {4}强度低于在QS中对于具有相同磁通密度的区域中获得的\ ion {4}。此外，随着磁通量的增加，CHS和QS之间强度的差异会增加。对于具有相等磁通密度的区域，QS线轮廓比CHS中测量的区域更为红移。此外，与QS不同的磁通量密度增加，CHS中测得的蓝色移位显示出增加。 QS和CHS中的非热速度随着磁通量的增加而增加。然而，尽管在较小的通量密度下，QS和CHS中没有观察到显着差异。使用这些结果，我们提出了一个统一模型，用于在QS和CHS中加热电晕以及太阳风的形成。
Coronal holes (CHs) are darker than quiet Sun (QS) when observed in coronal channels. This study aims to understand the similarities and differences between CHs and QS in the transition region using the \ion{Si}{4}~1394~Å line recorded by the Interface Region Imaging Spectrograph (IRIS) by considering the distribution of magnetic field measured by the Helioseismic and Magnetic Imager (HMI) onboard the Solar Dynamics Observatory (SDO). We find that \ion{Si}{4} intensities obtained in CHs are lower than those obtained in QS for regions with identical magnetic flux densities. Moreover, the difference in intensities between CHs and QS increases with increasing magnetic flux. For the regions with equal magnetic flux density, QS line profiles are more redshifted than those measured in CHs. Moreover, the blue shifts measured in CHs show an increase with increasing magnetic flux density unlike in the QS. The non-thermal velocities in QS, as well as in CHs, show an increase with increasing magnetic flux. However, no significant difference was observed in QS and CHs, albeit a small deviation at small flux densities. Using these results, we propose a unified model for the heating of the corona in the QS and in CHs and the formation of the solar wind.
