The disks around young stars are accretion disks.  Not only does this mean that material falls from the disk onto the star, but also that material is constantly being transported from one part of the disk to another, causing the disk to spread and heat and evolve with time.  We are conducting observational tests of some of the leading theories about how this evolution occurs.


Accretion Signatures

Disk Outer Edges
Clues to accretion history

Magnetic Fields from Submillimeter Polarimetry

Searching for evidence of magnetic field structure

Resolving Turbulence, Spectrally and Spatially

Testing predictions from MRI and other theories

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Debris Disks

Transition Disks

Accretion signatures


(Collaborative work)