The search for the smoking gun of disk dispersal via photoevaporative winds, leading to the formation of Type 1 Transition Disks, has until now failed to identify suitable diagnostics. Quantitative spectroscopy of YSOs to search for blue-shifted emission lines produced in the wind relies on an accurate characterisation of the thermochemical properties of the winds. A central ingredients for the chemical calculations is the dust content of the wind as micron sized grains provide the dominant opacity channel in the far-ultraviolet. Furthermore small particles are important players in the temperature balance of the gas via the photoelectric process. We will use realistic radiation-hydrodynamic models of photoevaporative winds coupled to dust evolution models for the underlying grain distribution in the disk, to calculate the dust entrainment in winds to feed to chemical models. The observability of the emission and scattering due to the dust grains in winds from edge-on disks, a potential new diagnostic, will be estimated for current and upcoming facilities (e.g. SPHERE, JWST) both for Herbig Ae stars and for their fainter T-Tauri counterparts.
DFG Programme
Research Units
International Connection
USA
