Magnetised winds in transition discs

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