Modeling of the Influence that Overlying Magnetic Fields have on the Initiation of Coronal Mass Ejections

Details Modeling of the Influence that Overlying Magnetic Fields have on the Initiation of Coronal Mass Ejections Modeling of the Influence that Overlying Magnetic Fields have on the Initiation of Coronal Mass Ejections

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufmsh41b1670o&link_type=abstract

American Geophysical Union, Fall Meeting 2009, abstract #SH41B-1670

Astronomy and Astrophysics

Astrophysics

[7513] Solar Physics, Astrophysics, And Astronomy / Coronal Mass Ejections, [7524] Solar Physics, Astrophysics, And Astronomy / Magnetic Fields

Scientific paper

We have been studying how the magnetic field profile of a flux rope, Coronal Mass Ejection (CME), model influences its initiation. A key finding is that a critical height, corresponding to a critical decay index n that quantifies the magnetic field profile exists where if the flux rope is allowed to evolve above this height it will become unstable and spontaneously erupt as soon as it exceeds this height. The value of the critical decay index in the limit of the flux rope model studied was found to be 2. Another interesting finding is that the width and peak of the corresponding eruptive acceleration profile can be controlled by the magnetic field strength and the rate of which the magnetic field decays immediately following the eruption onset. Poloidal flux injection also play a role in the eruption, it is found that the peak of the acceleration profile increases as the rate of poloidal flux injection increases during the acceleration phase. This kind of relationship may have some connection to flux conversion between the internal and ambient poloidal flux during the acceleration phase of the CME. The ideas presented here are applied to observations of a CME and it is shown that this mechanism, by exploring the magnetic field parameter space of the model, can approximately fit the observed acceleration profile.

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