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To understand the formation of quiescent solar prominences, the origin oftheir magnetic field structures, i.e., magnetic flux ropes (MFRs), must berevealed. We use three-dimensional magnetofriction simulations in a sphericalsubdomain to investigate the role of typical supergranular motions in thelong-term formation of a prominence magnetic field. Time-dependant horizontalsupergranular motions with and without the effect of Coriolis force aresimulated on the solar surface via Voronoi tessellation. The vortical motionsby the Coriolis effect at boundaries of supergranules inject magnetic helicityinto the corona. The helicity is transferred and accumulated along the polarityinversion line (PIL) as strongly sheared magnetic field via helicitycondensation. The diverging motions of supergranules converge opposite magneticpolarities at the PIL and drive the magnetic reconnection between footpoints ofthe sheared magnetic arcades to form an MFR. The magnetic network,negative-helicity MFR in the northern hemisphere, and fragmented-to-continuousformation process of magnetic dip regions are in agreement with observations.Although diverging supergranulations, differential rotation, and meridionalflows are included, the simulation without the Coriolis effect can not producean MFR or sheared arcades to host a prominence. Therefore Coriolis force is akey factor for helicity injection and the formation of magnetic structures ofquiescent solar prominences.

Formation of Quiescent Prominence Magnetic Field by Supergranulations