Planets are formed in the protoplanetary disks mostly probably through dust grain collisions and as time goes by larger and larger bodies are going to be formed toward planetesimals then eventually planets. However, this process is not straightforward as there are many barriers in front of planet formations. I will discuss the dynamics of dust and gas in the protoplanetary disks, then I will discuss grain growth, barriers in front of planetesimal formations and the possibles laboratory outcomes from grain grain collisions.

Finally, I will show the grain growth model that we are implementing into sphNG and will continue to explain the future improvements to our model.