Modelling magnetic flux emergence in the solar convection zone

摘要: Context. Bipolar magnetic regions are formed when loops of flux emerge at the solar photosphere. Magnetic buoyancy plays a crucial role in this emergence process, particularly larger scales. However it is not yet clear to what extent local convective motions influence evolution rising flux. Aims. Our aim investigate process simulation granular convection. In particular we determine circumstances under which enhances rate (which otherwise driven solely by upflows). Methods. We used three-dimensional numerical simulations, solving equations compressible magnetohydrodynamics horizontally-periodic Cartesian domain. A horizontal tube was inserted into fully developed hydrodynamic systematically varied initial field strength, thickness, entropy distribution along axis and Reynolds number. Results. Focusing upon low Prandtl number regime (Pm < 1) moderate number, find that always susceptible disruption some extent. However, stronger tubes tend maintain their structure more effectively than weaker ones. does enhance rates strongest cases, enhancement becomes pronounced increase width tube. This also case higher numbers, although generally lower these less dissipative simulations because much effective cases. These seem be relatively insensitive precise choice conditions: for given flow, determined primarily