In recent years, the Atacama Large Millimeter Array (ALMA) has given an
unprecedented look into the formation of stars and planets, but significant
mysteries still remain. One of the largest is how exactly the material of
the disk is removed and either built into planets or accreted onto the
central star. The turbulence is a key parameter in all theories of disk
dynamics, but remains extremely difficult to directly measure. This talk
will present a new method for characterizing disk turbulence for the
specific case of disks which are highly inclined and have visible rings,
and will present preliminary results for three protoplanetary disks.