The presence of elongations in active region (AR) polarities, called magnetic tongues, are mostly visible during their emergence phase. AR tilts have been measured thoroughly using long-term white-light (WL) databases, sometimes combined with magnetic field information. Since the influence of magnetic tongues on WL tilt measurements has not been taken into account before, we aim to investigate their role in tilt-angle values and to compare them with those derived from LOS magnetograms. We apply four methods to compute the tilt angle of generally bipolar ARs: one applies the k-means algorithm to WL data, a second one includes the magnetic field sign of the polarities to WL data, and a third one uses the magnetic flux-weighted center of each polarity. The tilt values computed in any of these ways are affected by the presence of magnetic tongues. Therefore, we apply the newly developed Core Field Fit Estimator (CoFFE) method to separate the magnetic flux in the tongues from that in the AR core. We compare the four computed tilt-angle values, as well as these with the ones reported in long-term WL databases. For ARs with low magnetic flux tongues the different methods report consistent tilt-angle values. But for ARs with high flux tongues there are noticeable discrepancies between all methods indicating that magnetic tongues affect differently WL and magnetic data. However, in general, CoFFE achieves a better estimation of the main bipole tilt because it removes both the effect of tongues as well as the emergence of secondary bipoles when it occurs in between the main bipole magnetic polarities.
Bayesian approach for modeling solar active region global magnetic parameters
上下文由于磁通量管的出现，太阳大气中出现了活动区（AR）。在视线（LOS）磁图中存在拉长的磁极性表明形成它们的磁通管中存在扭曲。这些被称为磁舌的极性伸长使在它们的出现阶段期间获得的AR特性的测量偏置（例如，它们的倾斜角和磁通量等）。特别是，获得一个很好的估计的倾斜角的演变起着关键作用，约束通量传输发电机模型。目的。在这项工作中，我们的目标是估计的扭曲的磁通管，或磁通绳，形成AR的定量比较所观察到的LOS磁图与合成的环形磁通量管模型。方法.为此，我们开发了一种贝叶斯推断方法来获得推断模型参数的统计分布。以NOAA AR 10268为例进行了验证。接下来，我们使用合成AR生成器来测试结果，以量化小尺度扰动对推断的参数分布的影响。结果我们的结论是，这种方法可以显着地消除磁舌的影响，所得出的AR全球特性，提供了一个更好的知识的内在属性的新兴磁通绳。结论.这些结果提供了一个框架，为未来的分析新兴AR的物理特性，使用贝叶斯统计。
Magnetic field dependence of bipolar magnetic region tilts on the Sun: Indication of tilt quenching
Indian Institute of Astrophysics（印度天体物理研究所）；Indian Institute of Technology (Banaras Hindu University)（印度理工学院（贝拿勒斯印度教大学））；Center of Excellence in Space Sciences India, IISER Kolkata（印度空间科学卓越中心，加尔各答印度科学与教育研究所）；Aryabhatta Research Institute of Observational Sciences（阿亚巴塔观测科学研究所以）
Investigation on the Relation between Active Regions' Compliance with Empirical Laws and Flare Productivity
CAS Key Laboratory of Geospace Environment, Department of Geophysics and Planetary Sciences, University of Science and Technology of China（中国科学院空间环境重点实验室，地球物理与行星科学学院，中国科学技术大学）；Mengcheng National Geophysical Observatory, University of Science and Technology of China（蒙城国家地球物理观测台，中国科学技术大学）；State Key Laboratory of Solar Activity and Space Weather, National Astronomical Observatories, Chinese Academy of Sciences（太阳活动与空间天气国家重点实验室，中国科学院国家天文台）；University of Chinese Academy of Sciences（中国科学院大学）；School of Space and Earth Sciences, Beihang University（航空航天大学空间与地球科学学院）；Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences（太阳活动重点实验室，中国科学院国家天文台）
Successive Injection of Opposite Magnetic Helicity: Evidence for Active Regions without Coronal Mass Ejections
磁螺旋度（MH）是磁场的扭曲和剪切的量度。MH通过光球足点运动注入活动区日冕，产生扭曲和剪切磁场。从螺旋度的守恒性质出发，证明了一个已经扭曲的磁绳（FR）不可避免地会随着MH的持续注入而爆发，以消除多余的日冕螺旋度。因此，理解光球螺旋度通量传输的性质和演化对于揭示耀斑/CME活动的强度至关重要。利用\textit{Helioseismic Magnetic Imager}的时间序列矢量磁图，我们研究了MH注入新兴AR 12257的演变。在这一AR的光球通量运动注入正螺旋度在前2.5天，随后负螺旋度。这种相反螺旋度的连续注入与平均无力扭转参数（$α_{av}$）的符号、磁舌的取向一致。此外，外推的AR磁结构表现出全球剪切没有扭曲的FR在AR的核心的转变。没有CME从这个AR发射，但C级耀斑活动主要是在演化期的后半段观察到的。具有MH注入符号反转的AR不利于具有过量日冕螺旋度的扭曲FR的形成，因此对于容易地识别无CME的AR是重要的。在这些AR的一个可能的情况是，当一个符号的螺旋度通量被相反的符号所取代，不同的连接与相反的剪切磁场经历重联在不同的尺度引起间歇性耀斑和增强的日冕加热。
