Description
Dust is an essential component of protoplanetary disks. The dust grains are the seeds of planet formation, they control the coupling with the magnetic field through the values of the non-ideal magnetohydrodynamics (MHD) resistivities and their continuum emission is extremely useful to observe star and disk forming regions. In the first part of this presentation, I will review recent results that we presented in Lebreuilly et al. 2020. In this work, we described in details the conditions for a gas and dust decoupling using the RAMSES code (Teyssier 2002) and its dust module (Lebreuilly et al., 2019). These conditions, when met, lead to the formation of protoplanetary disks that are initially significantly enriched in large dust grains. Protoplanetary disks and stars are not formed in isolation but rather in large turbulent clumps. To understand how the clump environment impacts the disk formation is crucial to determine their initial conditions. In that prospect, in the second part, I will introduce our new massive clump collapse simulations of 1000 solar mass gas-only clouds with and without non-ideal MHD (ambipolar diffusion) that aim to investigate protoplanetary disk formation within a self-consistent environment. These simulations, that resolve the disks up to the astronomical unit scale, allow us to obtain synthetic populations of early protoplanetary disks that can be compared with observed populations.
