disk

RadioImageofHD163296Disk 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.

Current Projects

Observing disk turbulence with ALMA

ALMA observations of disk structure

Planetesimal formation

Planet formation

Magnetohydrodynamic turbulence in protoplanetary disks

Athena code development

Past Projects

Mesoscale structures in MRI-driven turbulence

Outbursts in disks around young stars

 

 

 

 

 

JILA, University of Colorado
440 UCB
Boulder, CO 80309

contact1a1

303-546-0032

jbsimon.astro@gmail.com

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