Responsibility of a Filament Eruption for the Initiation of a Flare, CME, and Blast Wave, and its Possible Transformation into a Bow Shock

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• 作者：V. V. Grechnev (1)
  A. M. Uralov (1)
  I. V. Kuzmenko (2)
  A. A. Kochanov (1)
  I. M. Chertok (3)
  S. S. Kalashnikov (1)
  
• 关键词：Filament eruptions ; Flares ; Coronal mass ejections ; Shock waves ; Type II bursts
• 刊名：Solar Physics
• 出版年：2015
• 出版时间：January 2015
• 年：2015
• 卷：290
• 期：1
• 页码：129-158
• 全文大小：4,397 KB
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• 作者单位：V. V. Grechnev (1)
  A. M. Uralov (1)
  I. V. Kuzmenko (2)
  A. A. Kochanov (1)
  I. M. Chertok (3)
  S. S. Kalashnikov (1)
  
  1. Institute of Solar-Terrestrial Physics SB RAS, Lermontov St. 126A, Irkutsk, 664033, Russia
  2. Ussuriysk Astrophysical Observatory, Solnechnaya St. 21, Gornotaezhnoe, 692533, Primorsky Krai, Russia
  3. Pushkov Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation (IZMIRAN), Troitsk, Moscow, 142190, Russia
  
• ISSN：1573-093X

文摘

Multi-instrument observations of two filament eruptions on 24 February and 11?May 2011 suggest the following updated scenario for eruptive flare, coronal mass ejection (CME), and shock wave evolution. An initial destabilization of a filament results in stretching out of the magnetic threads belonging to its body that are rooted in the photosphere along the inversion line. Their reconnection leads to i)?heating of parts of the filament or its environment, ii)?an initial development of the flare cusp, arcade, and ribbons, iii) an increasing similarity of the filament to a curved flux rope, and iv) to its acceleration. Then the pre-eruption arcade enveloping the filament becomes involved in reconnection according to the standard model and continues to form the flare arcade and ribbons. The poloidal magnetic flux in the curved rope developing from the filament progressively increases and forces its toroidal expansion. This flux rope impulsively expands and produces a magnetohydrodynamical disturbance, which rapidly steepens into a shock. The shock passes through the arcade that expands above the filament and then freely propagates for some time ahead of the CME like a decelerating blast wave. If the CME is slow, then the shock eventually decays. Otherwise, the frontal part of the shock changes into the bow-shock regime. This was observed for the first time in the 24 February 2011 event. When reconnection ceases, the flux rope relaxes and constitutes the CME core–cavity system. The expanding arcade develops into the CME frontal structure. We also found that reconnection in the current sheet of a remote streamer forced by the shock passage results in a running flare-like process within the streamer responsible for a type?II burst. The development of dimming and various associated phenomena are discussed.