THE RELATION BETWEEN SOLAR ERUPTION TOPOLOGIES AND OBSERVED FLARE FEATURES. II. DYNAMICAL EVOLUTION
THE RELATION BETWEEN SOLAR ERUPTION TOPOLOGIES AND OBSERVED FLARE FEATURES. II. DYNAMICAL EVOLUTION
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DOI：
10.3847/0004-637x/817/1/43
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发表时间：
2016-01
期刊：
影响因子：
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通讯作者：
A. Savcheva;E. Pariat;S. McKillop;P. McCauley;E. Hanson;Y. Su;E. DeLuca
中科院分区：
文献类型：
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作者：
A. Savcheva;E. Pariat;S. McKillop;P. McCauley;E. Hanson;Y. Su;E. DeLuca
太阳物理学的一个长期目标是建立对太阳爆发的理解，并开发耀斑和日冕物质抛射（CME）预测模型。在本文中，我们继续我们的研究非线性力自由场（NLFFF）模型的比较的耀斑带演化的解的拓扑性质。特别是，我们表明，数据约束的NLFFF模型的三个爆发S形区域（SOL 2010 -04-08，SOL 2010 -08-07，和SOL 2012 -05-12）建立再现活动区磁场在耀斑前的状态可以呈现不稳定和后续序列的不稳定的解决方案产生准分界线层，符合耀斑带状演化观察SDO/AIA。我们开始与一个最适合的平衡模型的前耀斑活动区。然后，我们将轴向磁通添加到模型中的磁通绳，使其穿过稳定边界。在这一点上，磁摩擦代码不再收敛到平衡解。随着解的迭代，通量绳上升。我们解释的序列的磁摩擦步骤作为一个演变的活动区域的耀斑/CME开始。并与耀斑带的磁场解进行了比较。结果与标准耀斑/CME模型的三维扩展完全一致。我们的能力，捕捉必要的拓扑特征的耀斑活动区域的非动态磁摩擦代码强烈表明，耀斑前，大规模的拓扑结构被保存的通量绳变得不稳定，并解除。
A long-established goal of solar physics is to build understanding of solar eruptions and develop flare and coronal mass ejection (CME) forecasting models. In this paper, we continue our investigation of nonlinear forces free field (NLFFF) models by comparing topological properties of the solutions to the evolution of the flare ribbons. In particular, we show that data-constrained NLFFF models of three erupting sigmoid regions (SOL2010-04-08, SOL2010-08-07, and SOL2012-05-12) built to reproduce the active region magnetic field in the pre-flare state can be rendered unstable and the subsequent sequence of unstable solutions produces quasi-separatrix layers that match the flare ribbon evolution as observed by SDO/AIA. We begin with a best-fit equilibrium model for the pre-flare active region. We then add axial flux to the flux rope in the model to move it across the stability boundary. At this point, the magnetofrictional code no longer converges to an equilibrium solution. The flux rope rises as the solutions are iterated. We interpret the sequence of magnetofrictional steps as an evolution of the active region as the flare/CME begins. The magnetic field solutions at different steps are compared with the flare ribbons. The results are fully consistent with the three-dimensional extension of the standard flare/CME model. Our ability to capture essential topological features of flaring active regions with a non-dynamic magnetofrictional code strongly suggests that the pre-flare, large-scale topological structures are preserved as the flux rope becomes unstable and lifts off.