DIX Planetary Science Seminar
To form giant planets during protoplanetary disk lifetime, small micron sized particles must grow rapidly to larger grains. A full understanding of that process requires a detailed characterization of the radial and vertical structure of the gas-rich disks associated with young pre-main sequence stars. Multi-wavelengths observations of protoplanetary disks, for example in the millimeter and near-infrared, allow to probe two widely separated grain sizes that are differently affected by evolutionary mechanisms such as radial drift and vertical settling. In this talk, I will present constraints on both mechanisms using multi wavelengths observations, with a longer focus on disks seen edge-on. Highly inclined disks are of particular interest because they provide a unique point of view to unambiguously disentangle their vertical and radial dimensions. The modeling of multi-wavelength observations of such disks allows to identify high density regions, favorable for grain growth and planet formation, and to study the efficiency of planet formation in protoplanetary disks.