标题： 日冕磁绳的自动识别与追踪——第二部分：基于新数学形态学的磁绳提取方法及偏转分析 显示英文标题

标题： The Automatic Identification and Tracking of Coronal Flux Ropes -- Part II: New Mathematical Morphology-based Flux Rope Extraction Method and Deflection Analysis

摘要： 我们提出了一种用于太阳日冕磁场建模数据的磁通绳（FR）提取工具，该工具基于Wagner等人（2023年）的方法。我们将该方案应用于活动区AR12473和AR11176的磁场模拟。我们将该方法与其前身进行比较，并分别研究高度达200和300兆米的新提取FR的三维运动。提取方法基于扭曲参数以及多种数学形态算法，包括开变换和形态梯度。通过研究我们在其中提取FR平面内的圆度差异，我们突出了这些方法之间的不同之处。活动区的模拟使用了时变数据驱动的磁摩擦模型（TMFM；Pomoell等人，2019年）。我们通过追踪FR顶点在整个模拟时间跨度内来研究FR轨迹。我们证明这一升级后的技术为用户提供更多工具且对FR形状的先验假设更少，从而导致一组更准确的磁力线。传播分析表明，从AR12473爆发的FR展示了比AR11176 FR更强的动力学特性，并在其穿过区域时有显著偏转。AR11176的FR看起来更稳定，但仍存在明显的偏转。这证实了在这些低日冕高度上，即使在动力学较弱的情况下，FR的传播方向也会发生显著变化。建模结果也通过观测得到验证，AR12473确实具有动态性和爆发性，而AR11176仅在我们的模拟时间窗口之外表现出一次爆发。 显示英文摘要

摘要： We present a magnetic flux rope (FR) extraction tool for solar coronal magnetic field modelling data, which builds upon the methodology from Wagner et al. (2023). We apply the scheme to magnetic field simulations of active regions AR12473 and AR11176. We compare the method to its predecessor and study the 3D movement of the newly extracted FRs up to heights of 200 and 300 Mm, respectively. The extraction method is based on the twist parameter and a variety of mathematical morphology algorithms, including the opening transform and the morphological gradient. We highlight the differences between the methods by investigating the circularity of the FRs in the plane we extract from. The simulations for the active regions are carried out with a time-dependent data-driven magnetofrictional model (TMFM; Pomoell et al. (2019)). We investigate the FR trajectories by tracking their apex throughout the full simulation time span. We demonstrate that this upgraded methodology provides the user with more tools and less a-priori assumptions about the FR shape that, in turn, leads to a more accurate set of field lines. The propagation analysis yields that the erupting FR from AR12473 showcases stronger dynamics than the AR11176 FR and a significant deflection during its ascent through the domain. The AR11176 FR appears more stable, though there still is a notable deflection. This confirms that at these low coronal heights, FRs do undergo significant changes in the direction of their propagation even for less dynamic cases. The modelling results are also verified with observations, with AR12473 being indeed dynamic and eruptive, while AR11176 only features an eruption outside of our simulation time window.