I am utilizing both numerical simulations and radio observations to directly link theoretical predictions for the turbulent velocity structure of protoplanetary disks to observations with ALMA. By measuring the turbulent broadening component of molecular lines at different disk heights and radii, a 3D map of disk turbulence can be constructed. A direct comparison between observations and simulations will strongly constrain our understanding of how turbulence operates in these disks.
(Image by Hughes et al. 2011)
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