标题： 使用通量涌现模拟比较日冕洞和宁静太阳中的等离子体动力学 显示英文标题

标题： Comparison of plasma dynamics in Coronal Holes and Quiet Sun using flux emergence simulations

摘要： 本文通过2.5D MHD通量涌现模拟，比较了日冕洞（CHs）和宁静太阳（QS）中的等离子体动力学。 新兴通量与原有通量之间的磁重联导致形成具有热边界层的冷而密的等离子体团，以及速度为$\approx50$ km s$^{-1}$的热和冷喷流。 我们在探测过渡区和日冕温度的光谱线中进行光谱合成。 与QS相比，CHs在喷流（下流）期间表现出较低的强度、过量的上流（下流）以及较宽的谱线。 在喷流和下流期间，CHs中热谱线的速度和谱线宽度与z=0处的垂直磁场呈强正相关，而较冷谱线的强度仅显示弱相关性，这种现象在QS中并未出现。 在CH的喷流期间，我们发现Si IV中的上流与其他谱线中的上流（下流）相关（反相关），而CH中Si IV的下流与其他谱线中的上流（下流）相关（反相关），这与QS相比有所不同。 在下流期间，我们未发现Si IV与其他谱线速度之间有强相关性。 喷流期间的相关性是由于热喷流和冷喷流同时且同源产生的，而在下流阶段缺乏相关性表明热等离子体和冷等离子体发生了解耦。 这些结果表明，大气中与原有通量的通量涌现和重联支持了太阳风形成和日冕加热的统一情景。 显示英文摘要

摘要： This paper presents a comparison of plasma dynamics in Coronal Holes (CHs) and Quiet Sun (QS) through 2.5D MHD flux emergence simulations. The magnetic reconnection between the emerging and the pre-existing flux leads to the formation of cool, dense plasmoids with hot boundaries, and hot & cool jets with velocities $\approx50$ km s$^{-1}$. We perform spectral synthesis in spectral lines probing transition region and coronal temperatures. CHs show reduced intensities, excess upflows (downflows), and widths during the jetting (downflow) period when compared to QS. During the jetting and downflow periods, velocity and line width of the hot spectral lines in CHs show a strong positive correlation with the vertical magnetic field at z = 0, while the intensity of the cooler lines shows a weak correlation, which is not seen in QS. During the jetting period in CH, we find upflows in Si IV to be correlated (anti-correlated) with upflows (downflows) in other lines, and downflows in CH in Si IV to be correlated (anti-correlated) with upflows (downflows) in other lines when compared to QS. During downflow, we find no strong correlation between Si IV and other line velocities. The correlation during the jetting period occurs due to coincident, co-spatial origins of the hot and cool jet, while the lack of correlation during the downflow phase suggests a decoupling of hot and cool plasma. These results demonstrate that flux emergence and reconnection with pre-existing flux in the atmosphere support a unified scenario for solar wind formation and coronal heating.