Japan Geoscience Union Meeting 2019

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[E] Oral

P (Space and Planetary Sciences ) » P-EM Solar-Terrestrial Sciences, Space Electromagnetism & Space Environment

[P-EM12] Space Weather and Space Climate

Mon. May 27, 2019 10:45 AM - 12:15 PM A04 (TOKYO BAY MAKUHARI HALL)

convener:Ryuho Kataoka(National Institute of Polar Research), Antti A Pulkkinen(NASA Goddard Space Flight Center), Kanya Kusano(Institute for Space-Earth Environmental Research, Nagoya University), Kaori Sakaguchi(National Institute of Information and Communications Technology), Chairperson:Ryuho Kataoka(National Institute of Polar Research)

11:30 AM - 11:45 AM

[PEM12-10] The Role of a Tiny Brightening in a Huge Geo-effective Solar Eruption Leading to the St Patrick's Day Storm

*Yumi Bamba1,2, Satoshi Inoue1, Keiji Hayashi1,3,4 (1.Institute for Space-Earth Environmental Research/Nagoya University, 2.Institute if Space and Astronautical Science/Japan Aerospace Exploration Agency, 3.Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences, 4.State Key Laboratory for Space Weather, National Space Science Center, Chinese Academy of Sciences)

Keywords:St Patrick's Day Storm, Solar Flares, Filament Eruption, Hinode, Solar Dynamics Observatory

The largest magnetic storm in solar cycle 24 was caused by a fast coronal mass ejection (CME) that was related to a small C9.1 flare that occurred on 15 March 2015 in solar active region (AR) NOAA 12297. The purpose of this study is to understand the onset mechanism of the geo-effective huge solar eruption. We focused on the C2.4 flare that occurred prior to the C9.1 flare of the filament eruption. The magnetic field structure in the AR was complicated: there were several filaments including the one that erupted and caused the CME. We hence carefully investigated the photospheric magnetic field, brightenings observed in the solar atmosphere, and the three-dimensional coronal magnetic field extrapolated from nonlinear force-free field modeling, using data from Hinode and Solar Dynamics Observatory. We found three intriguing points : (1) There was a compact but noticeably highly twisted magnetic field structure that is represented by a small filament in the C2.4 flaring region, where a tiny precursor brightening was observed before the C2.4 flare. (2) The C2.4 flaring region is located in the vicinity of a foot point of the closed field that prohibits the filament from erupting. (3) The filament shows a sudden eruption after the C2.4 flare and accompanying small filament eruption. From our analysis, we suggest that a small magnetic disturbance that was represented by the tiny precursor brightening at the time of the C2.4 flare is related to the trigger of the huge filament eruption.