Abstract:
It is now commonly accepted that the formation of the building blocks of our Solar System might have occurred during the early phases of the protoplanetary disk. I will present studies of the self-consistent disk formation starting from the prestellar core collapse. We measure the disk properties, and our findings suggest that 1) the embedded disk structure and dynamics might be (unfortunately) more complicated than we thought and 2) the stellar mass accretion does not necessarily transit through the bulk of the disk as often naturally assumed. The collapse type numerical simulations are computationally challenging and render a wide search of the parameter space unfeasible. During the embedded class 0/1 phase, the close interaction with the envelope should not be neglected when considering the dynamics and evolution of the disk. We proposed a model for self-regulated disk formation, where the magnetic braking is moderated by the non-ideal MHD effects. The resulting disk radius is slowly varying for a wide range of physical parameters, which accounts for the observed small size (<50 au) of young disks. Putting the pieces together, an embedded disk is tightly connected to its envelope, while its global properties are not very sensitive to the prestellar core environment. A simplified view of the young embedded protoplanetary disk might still be possible, while our understanding of the way how a disk is built up within a collapsing envelope awaits further refinement.