Journal
JOURNAL OF FLUID MECHANICS
Volume 915, Issue -, Pages -Publisher
CAMBRIDGE UNIV PRESS
DOI: 10.1017/jfm.2021.108
Keywords
Benard convection; magneto convection; MHD turbulence
Categories
Funding
- Priority Programme SPP 1881 Turbulent Superstructures of the Deutsche Forschungsgemeinschaft (DFG) [VO 2331/3]
- DFG [VO 2331/1]
- CSC (China Scholarship Council)
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In geo- and astrophysics, low Prandtl number convective flows interact with magnetic fields. Static magnetic fields can stabilize flow fields, but self-organized convective flow structures can reach an optimal state where heat transport significantly increases. An increase in magnetic field strength beyond this state can lead to a reduction in heat and momentum transport due to Hartmann braking.
In geo- and astrophysics, low Prandtl number convective flows often interact with magnetic fields. Although a static magnetic field acts as a stabilizing force on such flow fields, we find that self-organized convective flow structures reach an optimal state where the heat transport significantly increases and convective velocities reach the theoretical free-fall limit, i.e. the maximum possible velocity a fluid parcel can achieve when its potential buoyant energy is fully converted into kinetic energy. Our measurements show that the application of a static magnetic field leads to an anisotropic, highly ordered flow structure and a decrease of the turbulent fluctuations. When the magnetic field strength is increased beyond the optimum state, Hartmann braking becomes dominant and leads to a reduction of the heat and momentum transport. The results are relevant for the understanding of magneto-hydrodynamic convective flows in planetary cores and stellar interiors in regions with strong toroidal magnetic fields oriented perpendicular to temperature gradients.
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