Fast Magnetic Wave Could Heat the Solar Low-beta Chromosphere
Fast Magnetic Wave Could Heat the Solar Low-beta Chromosphere
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DOI：
10.3847/2041-8213/ac10c7
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发表时间：
2021-07
期刊：
影响因子：
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通讯作者：
Yikang Wang;T. Yokoyama;H. Iijima
中科院分区：
文献类型：
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作者：
Yikang Wang;T. Yokoyama;H. Iijima
磁流体动力学（MHD）波是加热太阳色球层的候选者，尽管仍然不清楚哪种波的模式在加热中占主导地位。我们进行了二维辐射MHD模拟来研究MHD波在太阳色球安静区域的传播。我们利用激波前气体压力和磁压力之间的关系来识别激波的模式，并通过熵跳来计算它们相应的加热率，从而定量地了解色球层中的波加热过程。结果表明，快磁波对低β色球层的加热是重要的。低β快磁波是由高β快声波通过穿过均分层的模式转换产生的。通过激波传播方向与色球磁场之间的大攻角实现了有效的模式转换。
Magnetohydrodynamic (MHD) waves are candidates for heating the solar chromosphere, although it is still unclear which mode of the wave is dominant in heating. We perform two-dimensional radiative MHD simulation to investigate the propagation of MHD waves in the quiet region of the solar chromosphere. We identify the mode of the shock waves by using the relationship between gas pressure and magnetic pressure across the shock front and calculate their corresponding heating rate through the entropy jump to obtain a quantitative understanding of the wave-heating process in the chromosphere. Our result shows that the fast magnetic wave is significant in heating the low-beta chromosphere. The low-beta fast magnetic waves are generated from high-beta fast acoustic waves via mode conversion crossing the equipartition layer. Efficient mode conversion is achieved by large attacking angles between the propagation direction of the shock waves and the chromospheric magnetic field.