Yueh-Ning Lee (NTNU); Sébastien Charnoz (IPGP); Patrick Hennebelle (CEA Saclay)
It is now commonly accepted that the formation and processing of the building blocks of our Solar System, i.e., rocky materials, water ice, and carbon complex compounds, might have occurred, earlier than what was thought before, during the initial collapse of the prestellar core and the formation of the protoplanetary disk. Quite few existing works take into account the building phase of the protoplanetary disk when studying the formation and transport of refractory materials. Due to the complexity of this problem, a simplified hydrodynamic model has long been a convenient choice. We are now studying the self-consistent formation of the protoplanetary disks starting from the collapse that takes into account the environmental effects and large scale physics, including non-ideal magneto-hydrodynamic (MHD) effects that are relatively important at the disk scale, while not taken into account by many existing disk-formation models. With the help of numerical simulations that allow to follow the complex non-linear physics, we try to provide a working recipe for studies of the disk dynamics, thermal evolution of different gas and dust species, and their changes in chemical composition. I will address the properties of the disk formed in our numerical simulations, and compare the measured disk source function to the classical hydrodynamic model.