Title: MHD simulation of Solar Eruption from Active Region 11429 Driven by Photospheric Velocity Field Show Chinese title

Title: 太阳活动区11429光球速度场驱动的磁流体力学喷发模拟

Abstract: Data-driven simulation is becoming an important approach for realistically characterizing the configuration and evolution of solar active regions, revealing the onset mechanism of solar eruption events and hopefully achieving the goal of accurate space weather forecast, which is beyond the scope of any existing theoretical modelling. Here we performed a full 3D MHD simulation using the data-driven approach and followed the whole evolution process from quasi-static phase to eruption successfully for solar active region NOAA 11429. The MHD system was driven at the bottom boundary by photospheric velocity field, which is derived by the DAVE4VM method from the observed vector magnetograms. The simulation shows that a magnetic flux rope was generated by persistent photospheric flow before the flare onset and then triggered to erupt by torus instability. Our simulation demonstrates a high degree of consistency with observations in the pre-eruption magnetic structure, the time scale of quasi-static stage, the pattern of flare ribbons as well as the time evolution of magnetic energy injection and total unsigned magnetic flux. We further found that an eruption can also be initiated in the simulation as driven by only the horizontal components of photospheric flow, but a comparison of the different simulations indicates that the vertical flow at the bottom boundary is necessary in reproducing more realistically these observed features, emphasizing the importance of flux emergence during the development of this AR. Show Chinese abstract

Abstract: 数据驱动的模拟正成为真实表征太阳活动区结构和演化的重要方法，揭示太阳爆发事件的触发机制，并有望实现准确的空间天气预报，这是现有任何理论建模都无法企及的目标。 在这里，我们利用数据驱动的方法进行了全三维磁流体力学（MHD）模拟，并成功跟踪了太阳活动区 NOAA 11429 从准静态阶段到爆发的整个演化过程。 磁流体力学系统通过底部边界处的光球速度场驱动，该速度场由观测到的矢量磁图通过 DAVE4VM 方法推导而来。 模拟结果显示，在耀斑爆发前，由持续的光球流动生成了一个磁通量绳，随后由于磁陀螺不稳定性而触发爆发。 我们的模拟在爆发前的磁场结构、准静态阶段的时间尺度、耀斑带模式以及磁场能量注入和总无符号磁通量的时间演化方面与观测结果高度一致。 我们进一步发现，仅由光球流动的水平分量驱动时，模拟中也可以引发爆发，但不同模拟之间的对比表明，底部边界处的垂直流动对于更真实地再现这些观测特征是必要的，这强调了通量浮现在此类活动区发展中的重要性。