Sympathetic Solar Filament Eruptions on 2015 March 15

• Published in: arXiv.org
• Main Authors: Wang, Rui, Liu, Ying D, Zimovets, Ivan, Hu, Huidong, Dai, Xinghua, Yang, Zhongwei
• Format: Paper Journal Article
• Language: English
• Published: Ithaca Cornell University Library, arXiv.org 04.08.2016
• Subjects: Acceleration; Confining; Coronal mass ejection; Extrapolation; Filaments; Geomagnetism; Magnetic fields; Magnetic storms; Magnetism; Physics - Solar and Stellar Astrophysics; Potential fields; Solar corona; Solar cycle; Solar storms
• ISSN: 2331-8422
• DOI: 10.48550/arxiv.1608.01067

The 2015 March 15 coronal mass ejection as one of the two that together drove the largest geomagnetic storm of solar cycle 24 so far was associated with sympathetic filament eruptions. We investigate the relations between the different filaments involved in the eruption. A surge-like small-scale filament motion is confirmed as the trigger that initiated the erupting filament with multi-wavelength observations and using a forced magnetic field extrapolation method. When the erupting filament moved to an open magnetic field region, it experienced an obvious acceleration process and was accompanied by a C-class flare and the rise of another larger filament that eventually failed to erupt. We measure the decay index of the background magnetic field, which presents a critical height of 118 Mm. Combining with a potential field source surface extrapolation method, we analyze the distributions of the large-scale magnetic field, which indicates that the open magnetic field region may provide a favorable condition for F2 rapid acceleration and have some relation with the largest solar storm. The comparison between the successful and failed filament eruptions suggests that the confining magnetic field plays an important role in the preconditions for an eruption.