The coronal magnetic field evolution of 20 bipolar active regions (ARs) is simulated from their emergence to decay using the time-dependent nonlinear force-free field method of Mackay, Green, and van Ballegooijen (Astrophys. J. 729 , 97, 2011 ). A time sequence of cleaned photospheric line-of-sight magnetograms, which covers the entire evolution of each AR, is used to drive the simulation. A comparison of the simulated coronal magnetic field with the 171 and 193 Å observations obtained by the Solar Dynamics Observatory (SDO)/ Atmospheric Imaging Assembly (AIA), is made for each AR by manual inspection. The results show that it is possible to reproduce the evolution of the main coronal features such as small- and large-scale coronal loops, filaments and sheared structures for 80% of the ARs. Varying the boundary and initial conditions, along with the addition of physical effects such as Ohmic diffusion, hyperdiffusion and a horizontal magnetic field injection at the photosphere, improves the match between the observations and simulated coronal evolution by 20%. The simulations were able to reproduce the build-up to eruption for 50% of the observed eruptions associated with the ARs. The mean unsigned time difference between the eruptions occurring in the observations compared to the time of eruption onset in the simulations was found to be ≈5 hrs. The simulations were particularly successful in capturing the build-up to eruption for all four eruptions that originated from the internal polarity inversion line of the ARs. The technique was less successful in reproducing the onset of eruptions that originated from the periphery of ARs and large-scale coronal structures. For these cases global, rather than local, nonlinear force-free field models must be used. While the technique has shown some success, eruptions that occur in quick succession are difficult to reproduce by this method and future iterations of the model need to address this.

中文翻译：

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模拟双极活动区的日冕演化以研究通量绳的形成

使用 Mackay、Green 和 van Ballegooijen (Astrophys. J. 729 , 97, 2011 ) 的时间相关非线性无力场方法模拟 20 个双极活动区 (AR) 的日冕磁场演化从出现到衰减. 一个时间序列的清洁光球视线磁力图，涵盖了每个 AR 的整个演变，用于驱动模拟。模拟日冕磁场与太阳动力学天文台 (SDO)/大气成像组件 (AIA) 获得的 171 和 193 Å 观测值的比较，通过人工检查对每个 AR 进行。结果表明，可以重现 80% 的 AR 的主要日冕特征的演变，例如小型和大型日冕环、细丝和剪切结构。改变边界和初始条件，再加上物理效应，如欧姆扩散、超扩散和光球层的水平磁场注入，将观测结果与模拟日冕演化之间的匹配度提高了 20%。对于 50% 的观察到的与 AR 相关的喷发，模拟能够重现喷发的累积。与模拟中的喷发开始时间相比，观测中发生的喷发之间的平均无符号时间差约为 5 小时。对于源自 AR 内部极性反转线的所有四次喷发，模拟特别成功地捕捉到喷发的累积。该技术在再现起源于 AR 和大规模冠状结构外围的爆发方面不太成功。对于这些情况，必须使用全局而非局部非线性无力场模型。虽然该技术已显示出一些成功，但这种方法难以重现快速连续发生的喷发，模型的未来迭代需要解决这个问题。