Instabilities and Structures in Proto-Planetary disks

Rationale:
The meeting will address the evolution of the protoplanetary disks at the decoupling stage. The goal is to focus on:
- the possible formation of gaseous structures in the protoplanetary disks, particularly in the dead-zone, under various instabilities (baroclinic, or via Rossby or edge modes)
- their lifetime and evolution (stability, migration, collisions ....),
- their ability to capture the solid material and to survive once loaded.
Emphasis will be placed on the hydrodynamical aspects of the problem, without and with self-gravity, but MHD processes will not be forgotten. We will look also at the links with the experimental and numerical works performed in the physics of rotating flows and granular media.
The burning center of the discussions will be the possible (or impossible) routes toward planetesimals and planetary cores.

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