Monday, June 10, 2013 - 11:00am
"The first steps of planet formation in T-Tauri disks vs. Brown Dwarf disks"
Abstract. The first steps of planet formation imply the growth from ISM-like dust (micron-sized grains) to planetesimal-sized objects. At the beginning of this process, when particles are small enough to be well coupled to the gas, sticking collisions mainly occur due to Brownian motion and settling to the midplane. Once the dust particles have grown to sizes such that they decouple from the gas, radial/azimuthal drift and turbulent motion start to play an important role for the dust dynamics, which may lead to fragmentation collisions and rapid inward migration of the particles. Due to the different stellar properties, some of these phenomena occur differently for particles in disks around low-mass objects as Brown Dwarfs compared with typical Sun-like stars. In this talk, I will present how some processes as settling and radial drift differ for dust grains in BD and T-Tauri disks, and I will also show what are the recent results from millimeter-observations for both cases.