FORMATION OF MAGNETIC FLUX ROPES DURING CONFINED FLARING WELL BEFORE THE ONSET OF A PAIR OF MAJOR CORONAL MASS EJECTIONS
FORMATION OF MAGNETIC FLUX ROPES DURING CONFINED FLARING WELL BEFORE THE ONSET OF A PAIR OF MAJOR CORONAL MASS EJECTIONS
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DOI：
10.1088/0004-637x/809/1/34
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发表时间：
2015-08-10
影响因子：
4.9
通讯作者：
Vourlidas, Angelos
中科院分区：
文献类型：
--
作者：
Chintzoglou, Georgios;Patsourakos, Spiros;Vourlidas, Angelos
NOAA活动区域（AR） 11429是双超高速日冕物质抛射（cme）的来源。两次日冕物质抛射相隔不到一小时，第一次发生在2012年初的3月7日。这个AR满足了“超级活跃区域”的所有要求；即黑尔定律不相容和三角点磁构型。迄今为止，第24太阳周期中最大的风暴之一（D-st = - 143nt）与其中一个事件有关。磁通绳（MFRs）是日冕中扭曲的磁结构，在类似10 MK的热等离子体发射中最容易看到，通常被认为是喷发结构的核心。然而，它们在太阳大气中的“休眠”存在（即爆发之前）是一个悬而未决的问题。借助太阳动力学观测站（SDO）和日地关系观测站（STEREO）的多波长观测以及日冕磁场的非线性无力模型，我们的工作揭示了两个独立的、弱扭曲的磁通量系统，这表明爆发前的MFRs的存在最终成为了两次日冕抛射的种子。MFRs可能是在宿主ar11429的两次cme发生前一天的受限（即不会导致主要cme）耀斑和次耀斑事件中形成的。
NOAA active region (AR) 11429 was the source of twin super-fast coronal mass ejections (CMEs). The CMEs took place within an hour from each other, with the onset of the first taking place in the beginning of 2012 March 7. This AR fulfills all the requirements for a "super active region"; namely, Hale's law incompatibility and delta-spot magnetic configuration. One of the biggest storms of Solar Cycle 24 to date (D-st = -143 nT) was associated with one of these events. Magnetic flux ropes (MFRs) are twisted magnetic structures in the corona, best seen in similar to 10 MK hot plasma emission and are often considered the core of erupting structures. However, their "dormant" existence in the solar atmosphere (i.e., prior to eruptions), is an open question. Aided by multi-wavelength observations by the Solar Dynamics Observatory (SDO) and by the Solar Terrestrial Relations Observatory (STEREO) and a nonlinear force-free model for the coronal magnetic field, our work uncovers two separate, weakly twisted magnetic flux systems which suggest the existence of pre-eruption MFRs that eventually became the seeds of the two CMEs. The MFRs could have been formed during confined (i.e., not leading to major CMEs) flaring and sub-flaring events which took place the day before the two CMEs in the host AR 11429.