Mesoscale Disk Structures
Ionized disks are turbulent due to the magnetorotational instability (MRI). This turbulence generates structures on small scales (less than a vertical scale height), and has therefore been frequently studied in the local limit, focusing on a co-rotating disk patch.
By comparing these local disk patch simulations with global simulations, my colleagues and I have explored the formation and evolution of large scale structures that emerge from the disk turbulence.
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