Speaker
Description
Protoplanetary disk (PPD) winds play an important role in disk dispersal. Constraining disk wind models, along with accretion and jets, is necessary to understand its evolution, and eventually, planet formation. We trace these winds with optical forbidden emission lines of [OI], [SII], [NII], and [NeII] to estimate the wind kinematics and mass loss rates. The emission lines are comprised of multiple components that probably trace a different region in the system. At least one of these components was found to trace an ideal-MHD wind which was not considered in previous models. In addition, disk emission lines were found to be correlated to the accretion luminosity which means that the two processes are related. The correlation between emission lines and the FUV source (accretion) could provide a method for measuring the disk magnetic field.
