Protoplanetary discs (PPDs) are the birthplaces of planets and understanding how they evolve and eventually disperse is a central —and still open — challenge in astrophysics. In weakly ionized environments, the magnetic field is coupled to the gas through three non-ideal magnetohydrodynamic (MHD) effects — Ohmic resistivity, ambipolar diffusion, and the Hall effect — which together govern the disc's dynamics, suppressing turbulence and regulating angular momentum transport. Using 2.5D axisymmetric global simulations with the NIRVANA-III fluid code, I will present results from two complementary studies. First, transition discs (characterized by a large inner cavity) are examined under the influence of non-ideal MHD effects, with a focus on how mass is accreted across the cavity, whether density substructures can form, and how magnetic flux is transported. In the second part, I will focus on winds in full discs, where two distinct driving mechanisms are at play: magnetic winds and photoevaporative winds. The two are shown to originate at distinct radii, and their observational signatures are compared through synthetic spectral line diagnostics.
