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We conduct simulations of the inner regions of protoplanetary disks (PPDs) toinvestigate the effects of protostellar magnetic fields on their long-termevolution. We use an inner boundary model that incorporates the influence of astellar magnetic field. The position of the inner disk is dependent on the massaccretion rate as well as the magnetic field strength. We use this model tostudy the response of a magnetically truncated inner disk to an episodicaccretion event. Additionally, we vary the protostellar magnetic field strengthand investigate the consequences of the magnetic field on the long-termbehavior of PPDs. We use the fully implicit 1+1D TAPIR code which solves theaxisymmetric hydrodynamic equations self-consistently. Our model allows us toinvestigate disk dynamics close to the star and to conduct long-term evolutionsimulations simultaneously and includes the radial radiation transport in thestationary diffusion limit. We include stellar magnetic torques, the influenceof a pressure gradient, and a variable inner disk radius in the TAPIR code todescribe the innermost disk region in a more self-consistent manner and canshow that this approach alters the disk dynamics considerably compared to asimplified diffusive evolution equation, especially during outbursts. Theinfluences of a prescribed stellar magnetic field, local pressure gradients,and a variable inner disk radius result in a more consistent description of thegas dynamics in the innermost regions of PPDs. Combining magnetic torquesacting on the innermost disk regions with the long-term evolution of PPDsyields previously unseen results, whereby the whole disk structure is affectedover its entire lifetime. Additionally, we want to emphasize that a combinationof our 1+1D model with more sophisticated multi-dimensional codes could improvethe understanding of PPDs even further.

Time-dependent, long-term hydrodynamic simulations of the inner protoplanetary disk I: The importance of stellar magnetic torques