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Significant feedback from small-scale magnetic field and efficient energy transport in the solar convection zone

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Date and time:Ìý

Thursday, September 4, 2014 - 2:00pm

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ECCR 257

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Efficiency of small-scale dynamo in the solar convection zone is investigated in high resolution numerical calculations. The solar convection zone is filled with turbulent thermal convection. This convection transports the energy from the base of the convection zone to the solar surface. In addition, turbulent motion has ability to amplify magnetic field, i.e., dynamo. We significantly increase the numerical resolution with using a new method, the reduced speed of sound technique. Using higher resolution, the efficiency of dynamo is improved. Feedback of such strong magnetic field on fluid motion becomes strong. At the base of the convection zone, the root mean square velocity is reduced by 50%. In spite of significant reduction of the kinetic energy, the convective energy transport is not reduced much. In the talk, potential implications of these results for the recently raised issue of over-excited thermal convection in numerical calculations is discussed.