I am exploring how solid particles (roughly mm to cm in size) in planet forming disks clump together and collapse to planetesimal scales.
A very promising mechanism for this clumping is known as the streaming instability. Through state-of-the-art numerical simulations that couple particle gas drag physics to particle self-gravity, I am investigating issues related to planetesimal formation efficiency and the predicted size distribution of planetesimals.
Observing disk turbulence with ALMA
ALMA observations of disk structure
Magnetohydrodynamic turbulence in protoplanetary disks
Athena code development
Mesoscale structures in MRI-driven turbulence
Outbursts in disks around young stars