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Relaxation of writhe and twist of a bi-helical magnetic field View all abstracts by submitter

Axel Brandenburg   Submitted: 2003-07-10 20:59

In the past few years suggestions have emerged that the solar magnetic field might have a bi-helical component with oppositely polarized magnetic fields at large and small scales, and that the shedding of such fields may be crucial for the operation of the dynamo. It is shown that, if a bi-helical field is shed into the solar wind, positive and negative contributions of the magnetic helicity spectrum tend to mix and decay. Even in the absence of turbulence, mixing and decay can occur on a time scale faster than the resistive one provided the two signs of magnetic helicity originate from a single tube. In the presence of turbulence, positively and negatively polarized contributions mix rapidly in such a way that the ratio of magnetic helicity to magnetic energy is largest both at the largest scale and in the dissipation range. In absolute units the small scale excess of helical fields is however negligible.

Authors: T.A.Yousef, A. Brandenburg
Projects: None

Publication Status: Astron. Astrophys. (in press)
Last Modified: 2003-07-10 20:59
Go to main E-Print page  New dynamical mean field dynamo theory and closure approach   Doubly Helical Coronal Ejections from Dynamos and their Role in Sustaining the Solar Cycle  Edit Entry  Download Preprint  Submitter's Homepage Delete Entry 

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