Streaming Instabilities in Accreting and Magnetized Laminar Protoplanetary Disks

The streaming instability is one of the most promising pathways to formation planetesimals from pebbles. Understanding how this operates under realistic conditions expected in protoplanetary disks therefore crucial assess efficiency planet formation. Contemporary models show that magnetic fields are key driving gas accretion through large-scale, laminar stresses. However, effect such on has not been examined detail. To end, we study stability dusty, magnetized a disk. We find can be enhanced by passive torques and even persist absence global radial pressure gradient. In case, attributed azimuthal drift between dust gas, unlike classical instability, which driven drift. This suggests remain effective inside dust-trapping bumps accreting disks. When live vertical field considered, magneto-rotational damped feedback, while classic stabilized perturbations. also Alfv\'en waves destabilized dust-gas drift, but requires nearly ideal conditions. discuss possible implications these results for dynamics planetesimal