Data-driven MHD Simulation of Successive Solar Plasma Eruptions
Data-driven MHD Simulation of Successive Solar Plasma Eruptions
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DOI：
10.3847/1538-4357/abe414
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发表时间：
2021-01
期刊：
影响因子：
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通讯作者：
T. Kaneko;Sung-Hong Park;K. Kusano
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文献类型：
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作者：
T. Kaneko;Sung-Hong Park;K. Kusano
太阳耀斑和等离子体爆发是储存在等离子体大气中的磁能的突然释放。为了理解控制它们发生的物理机制，必须研究从光球到日冕的三维磁场。太阳光球磁场是可以观测到的，而日冕磁场是无法测量的。数据驱动模拟是日冕磁场推断的一种方法，该方法涉及光球磁场的时间序列观测数据和磁流体动力学模拟的底边界。我们开发了一种数据驱动的方法，该方法通过引入反向速度场，可以在模拟的底部边界再现观测矢量磁场的时间演变。该速度场是通过反求解感应方程并进行适当的规范变换得到的。利用这种方法，我们对2017年11月太阳动力学观测站和太阳磁活动望远镜观测到的连续小喷发进行了数据驱动模拟。模拟很好地再现了相反极性磁块之间的会聚运动，显示了螺旋通量绳的连续形成和喷发。
Solar flares and plasma eruptions are sudden releases of magnetic energy stored in the plasma atmosphere. To understand the physical mechanisms governing their occurrences, three-dimensional magnetic fields from the photosphere up to the corona must be studied. The solar photospheric magnetic fields are observable, whereas the coronal magnetic fields cannot be measured. One method for inferring coronal magnetic fields is performing data-driven simulations, which involves time-series observational data of the photospheric magnetic fields with the bottom boundary of magnetohydrodynamic simulations. We developed a data-driven method in which temporal evolutions of the observational vector magnetic field can be reproduced at the bottom boundary in the simulation by introducing an inverted velocity field. This velocity field is obtained by inversely solving the induction equation and applying an appropriate gauge transformation. Using this method, we performed a data-driven simulation of successive small eruptions observed by the Solar Dynamics Observatory and the Solar Magnetic Activity Telescope in 2017 November. The simulation well reproduced the converging motion between opposite-polarity magnetic patches, demonstrating successive formation and eruptions of helical flux ropes.