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In the past few years suggestions have emerged that the solar magnetic fieldmight have a bi-helical component with oppositely polarized magnetic fields atlarge and small scales, and that the shedding of such fields may be crucial forthe operation of the dynamo. It is shown that, if a bi-helical field is shedinto the solar wind, positive and negative contributions of the magnetichelicity 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 oneprovided the two signs of magnetic helicity originate from a single tube. Inthe presence of turbulence, positively and negatively polarized contributionsmix rapidly in such a way that the ratio of magnetic helicity to magneticenergy is largest both at the largest scale and in the dissipation range. Inabsolute units the small scale excess of helical fields is however negligible.Comment: 6 pages, 9 figures, to be published in Astron. Astrophy

Relaxation of writhe and twist of a bi-helical magnetic field