We present the first results of the treatment of grain growth in our 3D, two-fluid (gas+dust) SPH code describing protoplanetary disks. We implement a scheme able to reproduce the variation of grain sizes caused by a variety of physical processes and test it with the analytical expression of grain growth given by Stepinski & Valageas (1997) in simulations of a typical T Tauri disk around a one solar mass star. The results are in agreement with a turbulent growing process and validate the method. We are now able to simulate the grain growth process in a protoplanetary disk given by a more realistic physical description, currently under development. We discuss the implications of the combined effect of grain growth and dust vertical settling and radial migration on subsequent planetesimal formation.
Exoplanets: detection, formation and dynamics: proceedings of the International Astronomical Union Symposium 249, Suzhou, China, 22-26 October 2007 / Yi-Sui Sun, Sylvio Ferraz Mello and Ji-Lin Zhou (eds.),
Vol. 3, no. (2008), pp. 385-388