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Protoplanetary discs (PPDs) are cold, dense and weakly ionised environmentsthat witness the planetary formation. Among these discs, transition discs (TDs)are characterised by a wide cavity in the dust and gas distribution. Despitethis lack of material, many TDs strongly accrete onto their central star,possibly indicating that a mechanism is driving fast accretion in TDs cavities.The presence of radially extended 'dead zones' in PPDs recently revived theinterest in magnetised disc winds (MDWs), where accretion is driven by a largemagnetic field. We propose that TDs could be subject to similar winds,explaining their fast-accreting and long-lived cavities. We present the resultsof the first 2.5D global numerical simulations of TDs harbouring MDWs using thePLUTO code. We impose a cavity in the gas distribution and consider a power lawdistribution for the large-scale magnetic field strength. We assume weaklyionised discs subject to ambipolar diffusion, as expected in this range ofdensities and temperatures. Our simulated TDs reach a steady state with aninner cavity and an outer 'standard' disc. The accretion rates remainapproximately constant through the entire discs, reaching$10^{-7}~M_\odot/\text{yrs}^{-1}$ for typical surface density values. The MDWlaunched from the cavity is more magnetised with a much larger lever arm thanthe MDW launched from the outer disc. The material in the cavity is accreted atsonic velocities, and the cavity itself is rotating at 70% of the Keplerianvelocity due to the efficient magnetic braking imposed by the MDW. Overall, ourcavity matches the dynamical properties of an inner jet emitting disc (JED) andof magnetically arrested discs (MADs) in black hole physics. Finally, kinematicdiagnostics (wind speeds, orbital and accretion velocities) could disentangleclassical photo-evaporation from MDW models.

Magnetised Winds in Transition Discs I: 2.5D Global Simulations