Meridional circulation dynamics in a cyclic convective dynamo

摘要: Surface observations indicate that the speed of solar meridional circulation in photosphere varies anti-phase with cycle. The current explanation for source this variation is inflows into active regions alter global surface pattern circulation. When these localized are integrated over a full hemisphere, they contribute to slowing down axisymmetric poleward horizontal component. behavior large-scale flow deep inside convection zone remains largely unknown. Present helioseismic techniques not sensitive enough capture dynamics weak flow. Moreover, large time integration needed map zone, also masks some possible on shorter timescales. In work we examine emerges from 3D MHD simulation zone. Our aim assess and quantify where cyclic magnetic field can reach considerable strength. analyses morphology amplitude both highly influenced by via impact torques angular momentum distribution. A dynamic feature induced development prominent upward at mid-latitudes lower occurs near equatorward edge toroidal bands peaks during cycle maximum. Globally, dynamo-generated drives variations flow, stark contrast conventional kinematic flux transport view being advected passively