Turbulence is a key ingredient in the disk evolution and planet formation. However, the origin of the low level of turbulence recently observed in protoplanetary disks is not yet well understood.
The Vertical Shear Instability (VSI) is a candidate to be responsible for the hydrodynamic turbulence in the outer regions of the disk.
Via 3D global hydrodynamical simulations, we study the...
In the early stages of a protoplanetary disk, when its mass is a significant fraction of its star's, turbulence generated by gravitational instability (GI) should feature significantly in the disk's evolution. At the same time, the disk may be sufficiently ionised for magnetic fields to play some role in the dynamics.
Though usually neglected, the impact of magnetism on the GI may be...
Massive protostellar discs are the sibling circumstellar structures of protoplanetary accretion discs. They form, evolve as a scaled-up version of the surroundings of low-mass stars and both formation mechanisms are unified within the so-called burst mode of star formation. This picture naturally links the development of gravitational instabilities in centrifugally balanced accretion discs to...
I will present the results on the evolution of dust particles in self-gravitating disks residing in a gravitoturbulent state, when heating due to shocks of density waves balances cooling. It is well known that density structures in the gaseous component of the disk induced by self-gravity (gravitational instability) can trap dust efficiently enough, so that the dust component itself undergoes...
