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15 mins
Rodion Stepanov, Irina Mizeva, Peter Frick
Session: Magnetohydrodynamics 2
Session starts: Tuesday 25 August, 15:00
Presentation starts: 16:30
Room: Room F

Rodion Stepanov ()
Irina Mizeva ()
Peter Frick ()

Magnetohydrodynamic (MHD) turbulence is an important part of astrophysical processes, which gives rise to global cosmic magnetic fields. Over the last few decades, the peculiarities of MHD turbulence have attracted the interest of researchers in astrophysics and fluid dynamics, significant attention has been paid to the role of magnetic helicity in fully developed MHD turbulence. Magnetic helicity, together with the energy and cross-helicity, is one of the three integrals of motion in ideal MHD. We show that oppositely directed fluxes of energy and magnetic helicity coexist in the inertial range in fully developed magnetohydrodynamic (MHD) turbulence with small-scale sources of magnetic helicity. Using a helical shell model of MHD turbulence, we study the high Reynolds number magnetohydrodynamic turbulence with well separated scales of energy input, magnetic helicity input and magnetic helicity sink. We obtain three inertial ranges with different scaling properties. In a short range of scales larger than the forcing scale of magnetic helicity, a bottleneck-like effect appears, which results in a local reduction of the spectral slope. The slope changes in a domain with a high level of relative magnetic helicity, which determines that part of the magnetic energy related to the helical modes at a given scale. In the infrared part of the spectra we observe simultaneous inverse cascade of energy and magnetic helicity. Our results indicate that a large-scale dynamo can be affected by the magnetic helicity generated at small scales. The kinetic helicity, in particular, is not involved in the process at all.