Disk Structure with ALMA
As a follow-up to my work on quantifying observational signatures of disk turbulence (described here), I am also determining the observability of large scale structures induced via mechanisms such as the magnetorotational instability (MRI). In the case of the MRI, large scale, axisymmetric structures, called "zonal flows', emerge and lead to enhanced dust concentrations. A simulated image in the dust continuum is shown on the left. Zonal flows could be responsible for producing the structure of disks like HL Tau.
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