Two-Step Filament Eruption During 14-15 March 2015

被引：28

作者：

Chandra, R. ^{[1
]}

Filippov, B. ^{[2
]}

Joshi, R. ^{[1
]}

Schmieder, B. ^{[3
]}

机构：

[1] Kumaun Univ, Dept Phys, DSB Campus, Naini Tal 263001, India

[2] Russian Acad Sci, Pushkov Inst Terr Magnetism Ionesphere & Radio Wa, Moscow, Russia

[3] Observ Paris, LESIA, UMR8109, CNRS, F-92195 Meudon, France

来源：

SOLAR PHYSICS | 2017年 / 292卷 / 06期

关键词：

Sun; -; filament; corona; Sun-jets; magnetic; CORONAL MASS EJECTIONS; GEOMAGNETIC STORM; SOLAR; PROMINENCES; MODEL; MECHANISM; FLARES; PHASE; EUV;

D O I：

10.1007/s11207-017-1104-5

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present here an interesting two-step filament eruption during 14 -15 March 2015. The filament was located in NOAA AR 12297 and associated with a halo Coronal Mass Ejection (CME). We use observations from the Atmospheric Imaging Assembly (AIA) and Heliospheric Magnetic Imager (HMI) instruments onboard the Solar Dynamics Observatory (SDO), and from the Solar and Heliospheric Observatory (SOHO) Large Angle and Spectrometric Coronagraph (LASCO). We also use Ha data from the Global Oscillation Network Group (GONG) telescope and the Kanzelhoehe Solar Observatory. The filament shows a first step eruption on 14 March 2015 and it stops its rise at a projected altitude approximate to 125 Mm on the solar disk. It remains at this height for approximate to 12 hrs. Finally it erupts on 15 March 2015 and produces a halo CME. We also find jet activity in the active region during both days, which could help the filament de-stabilization and eruption. The decay index is calculated to understand this two-step eruption. The eruption could be due to the presence of successive instability-stability-instability zones as the filament is rising.

引用

页数：15

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