In this work, we present results of a time-dependent data-driven numerical simulation developed to study the dynamics of coronal active region magnetic fields. The evolving boundary condition driving the model, the photospheric electric field, is inverted using a time sequence of vector magnetograms as input. We invert three distinct electric field datasets for a single active region. All three electric fields reproduce the observed evolution of the normal component of the magnetic field. Two of the datasets are constructed so as to match the energy input into the corona to that provided by a reference estimate. Using the three inversions as input to a time-dependent magnetofrictional model, we study the response of the coronal magnetic field to the driving electric fields. The simulations reveal the magnetic field evolution to be sensitive to the input electric field despite the normal component of the magnetic field evolving identically and the total energy injection being largely similar. Thus, we demonstrate that the total energy injection is not sufficient to characterize the evolution of the coronal magnetic field: coronal evolution can be very different despite similar energy injections. We find the relative helicity to be an important additional metric that allows one to distinguish the simulations. In particular, the simulation with the highest relative helicity content produces a coronal flux rope that subsequently erupts, largely in agreement with extreme-ultraviolet imaging observations of the corresponding event. Our results suggest that time-dependent data-driven simulations that employ carefully constructed driving boundary conditions offer a valuable tool for modeling and characterizing the evolution of coronal magnetic fields.

中文翻译：

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使用能量优化光球电场对活动区域演化进行时间相关的数据驱动建模

在这项工作中，我们展示了为研究日冕活动区磁场动力学而开发的时间相关数据驱动数值模拟的结果。使用矢量磁图的时间序列作为输入来反演驱动模型的不断变化的边界条件（光球电场）。我们反转单个活动区域的三个不同的电场数据集。所有三个电场都再现了观察到的磁场法向分量的演化。构建两个数据集，以便将输入日冕的能量与参考估计提供的能量相匹配。使用这三个反演作为随时间变化的磁摩擦模型的输入，我们研究了日冕磁场对驱动电场的响应。模拟表明，尽管磁场的法向分量演化相同且总能量注入基本相似，但磁场演化对输入电场敏感。因此，我们证明总能量注入不足以表征日冕磁场的演化：尽管能量注入相似，日冕演化可能非常不同。我们发现相对螺旋度是一项重要的附加指标，可以让人们区分模拟。特别是，具有最高相对螺旋度内容的模拟产生了随后爆发的日冕磁通绳，这在很大程度上与相应事件的极紫外成像观测结果一致。我们的结果表明，采用精心构建的驱动边界条件的时间相关数据驱动模拟为建模和表征日冕磁场的演化提供了有价值的工具。