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Formation of Magnetic Flux Ropes during Confined Flaring Well Before the Onset of a Pair of Major Coronal Mass Ejections View all abstracts by submitter

Georgios Chintzoglou   Submitted: 2015-07-06 18:46

NOAA Active Region (AR) 11429 was the source of twin super-fast Coronal Mass Ejections (CMEs). The CMEs took place within a hour from each other, with the onset of the first taking place in the beginning of March 7, 2012. This AR fulfills all the requirements for a ``super active region''; namely, Hale's law incompatibility and a δ-spot magnetic configuration. One of the biggest storms of Solar Cycle 24 to date (Dst=-143 nT) was associated with one of these events. Magnetic Flux Ropes (MFRs) are twisted magnetic structures in the corona, best seen in ~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 (SDO/HMI/AIA and STEREO EUVI B) and a Non-Linear Force-Free (NLFFF) 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.

Authors: Georgios Chintzoglou, Spiros Patsourakos, Angelos Vourlidas
Projects: None

Publication Status: In print; Astrophysical Journal (ApJ)
Last Modified: 2015-07-08 12:56
Go to main E-Print page  Calibration of Hinode/XRT for Coalignment  Optimal Electron Energies for Driving Chromospheric Evaporation in Solar Flares  Edit Entry  Download Preprint  Delete Entry 

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