A Multiple Flare Scenario where the Classic Long-Duration Flare Was Not the Source of a CME

A Multiple Flare Scenario where the Classic Long-Duration Flare Was Not the Source of a CME
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DOI:
10.1007/s11207-007-0260-4
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发表时间:
2007-03
期刊:
影响因子:
2.8
通讯作者:
C. P. Goff;L. Driel-Gesztelyi;L. Driel-Gesztelyi;L. Driel-Gesztelyi;P. Démoulin;J. Culhane;S. Matthews;L. Harra;C. Mandrini;K. Klein;H. Kurokawa
C. P. Goff;L. Driel-Gesztelyi;L. Driel-Gesztelyi;L. Driel-Gesztelyi;P. Démoulin;J. Culhane;S. Matthews;L. Harra;C. Mandrini;K. Klein;H. Kurokawa
中科院分区:
物理与天体物理3区
文献类型:
--
作者:
C. P. Goff;L. Driel-Gesztelyi;L. Driel-Gesztelyi;L. Driel-Gesztelyi;P. Démoulin;J. Culhane;S. Matthews;L. Harra;C. Mandrini;K. Klein;H. Kurokawa

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2004年1月20日,在NOAA 10540观测到一系列的耀斑(GOES M、M和C级)和CME。以II型、III型和N型爆发形式出现的射电观测与这些事件有关。我们使用来自TRACE、EIT、来自Kwasan的Hα图像、MDI磁图和GOES的综合观测来了解这一事件的复杂发展。与标准解释相反,我们得出结论,前两个脉冲耀斑是CME发射过程的一部分,而随后的长时间事件耀斑仅代表恢复阶段。观测结果表明,耀斑带不仅分离,而且沿磁倒转线移动,使磁重联逐步向邻近的磁管进行。我们的结论是,在剪切拱廊中的“系绳切割”重连逐渐将其转变为扭曲的磁通管,变得不稳定,导致CME。我们认为第三次耀斑是一个持续时间较长的事件,是经典的双带耀斑与膨胀的CME结构与邻近磁场之间强制重联后的弛缓过程的结合。
A series of flares (GOES class M, M and C) and a CME were observed in close succession on 20 January 2004 in NOAA 10540. Radio observations, which took the form of types II, III and N bursts, were associated with these events. We use the combined observations from TRACE, EIT, Hα images from Kwasan, MDI magnetograms and GOES to understand the complex development of this event. Contrary to a standard interpretation, we conclude that the first two impulsive flares are part of the CME launch process while the following long-duration event flare represents simply the recovery phase. Observations show that the flare ribbons not only separate but also shift along the magnetic inversion line so that magnetic reconnection progresses stepwise to neighboring flux tubes. We conclude that “tether cutting” reconnection in the sheared arcade progressively transforms it to a twisted flux tube, which becomes unstable, leading to a CME. We interpret the third flare, a long-duration event, as a combination of the classical two-ribbon flare with the relaxation process following forced reconnection between the expanding CME structure and neighboring magnetic fields.