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On the Role of the Background Overlying Magnetic Field in Solar Eruptions View all abstracts by submitter

Alexander Nindos   Submitted: 2012-02-16 03:35

The primary constraining force that inhibits global solar eruptions isprovidedby the overlying background magnetic field. Using magnetic field datafrom both the Helioseismic and Magnetic Imager aboard Solar DynamicsObservatoryand the spectropolarimeter of the Solar Optical Telescope aboard Hinode,we study the long-term evolution of the background field in activeregionAR11158 that produced three major coronal mass ejections (CMEs). The CMEformation heights were determined using EUV data. We calculated thedecayindex -(Z/B)(dB/dz_ of the magnetic field B (i.e. how fast the fielddecreases with height, z) related to each event from the time of theactive region emergenceuntil well after the CMEs. At the heights of CME formation, the decayindices were 1.1-2.1. Prior to two of the events, there were extendedperiods (ofmore than 23 hours) where the related decay indices at heights abovethe CMEformation heights either decreased (up to -15%) or exhibited smallchanges. Thedecay index related to the third event increased (up to 118%) atheights above20 Mm within an interval that started 64 hours prior to the CME. Themagneticfree energy and the accumulated helicity into the corona contributedthe mostto the eruptions by their increase throughout the flux emergence phase(by factorsof more than 5 and more than two orders of magnitude, respectively). Ourresults indicate that the initiation of eruptions does not dependcritically on thetemporal evolution of the variation of the background field with height.

Authors: A. Nindos, S. Patsourakos, T. Wiegelmann
Projects: None

Publication Status: ApJ (Letters), in press
Last Modified: 2012-02-17 08:42
Go to main E-Print page  How to optimize nonlinear force-free coronal magnetic field extrapolations from SDO/HMI vector magnetograms?  Magnetic reconnection from a multiscale instability cascade  Edit Entry  Download Preprint  Delete Entry 

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