Astronomy and Astrophysics – Astrophysics
Scientific paper
2006-01-23
Astron.Nachr. 327 (2006) 461-468
Astronomy and Astrophysics
Astrophysics
8 pages, 5 figures, talk given in Bologna, August 2006, proceedings of "The Origin and Evolution of Cosmic Magnetism", Astron.
Scientific paper
10.1002/asna.200610558
Some common properties of helical magnetic fields in decaying and driven turbulence are discussed. These include mainly the inverse cascade that produces fields on progressively larger scales. Magnetic helicity also restricts the evolution of the large scale field: the field decays less rapidly than a non-helical field, but it also saturates more slowly, i.e. on a resistive time scale if there are no magnetic helicity fluxes. The former effect is utilized in primordial field scenarios, while the latter is important for successfully explaining astrophysical dynamos that saturate faster than resistively. Dynamo action is argued to be important not only in the galactic dynamo, but also in accretion discs in active galactic nuclei and around protostars, both of which contribute to producing a strong enough seed magnetic field. Although primordial magnetic fields may be too weak to compete with these astrophysical mechanisms, such fields could perhaps still be important in producing polarization effects in the cosmic background radiation.
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