发表机构
National Institute of Technology Calicut; Indian Institute of Astrophysics（国立卡尔卡提理工学院; 印度天体物理研究所）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究分析第24太阳活动周极大期35个暗条的形态，发现77%遵循半球手性偏好，且所有检查的日冕拱符合螺旋度判据，未发现违反手性偏好与爆发倾向的关联。
AI 中文摘要
太阳大气中的暗条是由磁场支撑、抵抗重力作用的等离子体结构。由于缺乏对其磁场的直接观测，分析其磁结构具有挑战性。然而，通过多波段强度观测，可以推断其形态。我们在第24太阳活动周极大期识别出35个太阳暗条。为确定其手性，我们分析了Hα强度观测。利用日冕紫外强度图像，我们还确定了相关日冕拱的倾斜度。此外，根据邻近活动区，我们依据附近光球磁场强度将暗条分为宁静暗条或活动暗条。我们随时间跟踪每个暗条以估算其特性。基于观测到的旋向，27个（77%）暗条在所有类别中遵循半球手性偏好。我们检查了与19个暗条相连的日冕拱的倾斜度，它们均符合半球螺旋度判据。通过整合倾斜度和旋向，还确定了16个暗条的形态。其中两个暗条具有剪切拱形态，十四个具有磁绳形状。此外，通过分析日冕拱倾斜度和暗条倒刺旋向随时间的变化，我们考察了暗条磁结构的变化。进一步，我们研究了在观测期间表现出特殊特征的选定暗条的时间演化。最后，我们调查了这些暗条的爆发特征。我们未发现因不遵循半球手性偏好而更可能爆发的暗条。
英文摘要
Filaments in the solar atmosphere are plasma structures held aloft by magnetic fields, counteracting the pull of gravity. Analyzing their magnetic structure is challenging due to the lack of direct observations of their magnetic fields. However, through multi-wavelength intensity observations, one can infer their morphology. We identified 35 solar filaments during the maximum period of the solar cycle 24. In order to ascertain their chirality, we analyzed H$α$ intensity observations. Using coronal ultraviolet intensity images, we also determined the skewness of the related coronal arcades. Furthermore, based on adjacent active regions, we classified filaments as quiescent or active, according to strength of nearby photospheric magnetic fields. We followed every filament over time to estimates their characteristics. The hemispheric chirality preference is followed by 27 (77%) filaments across all categories, based on observed bearing sense. We examined the skewness of the coronal arcades connected to 19 filaments, and they all complied with the hemisphere helicity criterion. The morphology of 16 filaments was also ascertained by integrating the skewness and bearing sense. There were two filaments with sheared arcade morphology and fourteen with flux rope shape. Additionally, by analyzing the changes in the skewness of coronal arcades and the bearing sense of filament barbs over time, we examined the variation in filament magnetic structure. Further, we examine the temporal evolution of selected filaments, which exhibit peculiar characteristics during the observational period. Lastly, we investigated the eruptive characteristics of these filaments. We did not find filaments that are more likely to explode because they do not adhere to the hemispheric chirality preference.
Comments14 pages, 8 figures, 2 tables, Accepted for Publication in The Astrophysical Journal (ApJ)
