E-Print Archive

There are 4035 abstracts currently viewable.


Search:

Advanced Search
Options
Main Page Add New E-Print Submitter
Information
Feedback
News Help/FAQ About Preferences
Manage Key Phrase
Notification
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 

Key
Go to main E-Print pageGo to main E-Print page.
Previous AbstractPrevious Abstract.
Next AbstractNext Abstract.
Download PreprintDownload Preprint.
Submitter's HomepageSubmitters Homepage.
Edit EntryEdit Entry.
View All Abstracts By SubmitterView all abstracts by submitter.
Delete AbstractDelete abstract.

Latest Entries
Why Does the Solar Corona Abnormally Rotate Faster Than the Photosphere?
Impacts On Proton Fluxes Observed During Different Interplanetary Conditions
Coronal Loop Seismology Using Standing Kink Oscillations With a Lookup Table
Data-Optimized Coronal Field Model: I. Proof of Concept
Coronal Bright Points
Difference of source regions between fast and slow coronal mass ejections
Invited Review: Signatures of Magnetic Flux Ropes in the Low Solar Atmosphere Observed in High Resolution
Do Kepler superflare stars really include slowly-rotating Sun-like stars ? - Results using APO 3.5m telescope spectroscopic observations and Gaia-DR2 data -
Magnetically Induced Current Piston for Generating Extreme-ultraviolet Fronts in the Solar Corona
Magnetic Field Dynamics and Varying Plasma Emission in Large-scale Coronal Loops
Nonlinear Evolution of Ion Kinetic Instabilities in the Solar Wind
What determines the X-ray intensity and duration of a solar flare?
Fast Magnetoacoustic Wave Trains with Time-dependent Drivers
Three-dimensional reconstruction of CME-driven shock-streamer interaction from radio observations: a different take on the diagnostics of coronal magnetic fields
The soft X-ray spectrometer polarimeter SolpeX
Variable emission mechanism of a Type IV radio burst
Inference of magnetic field strength and density from damped transverse coronal waves
Frequency-Distance Structure of Solar Radio Sources Observed by LOFAR
The birth of a coronal mass ejection
Properties of slow magnetoacoustic oscillations of solar coronal loops by multi-instrumental observations

Related Pages
MSU Solar Physics.
Max Millennium Science Mail Archive.
Max Millennium Message of the Day Mail Archive.
Max Millennium Flare Catalog

Archive Maintainer
Alisdair Davey



© 2003 Solar Physics Group - Montana State University