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| = Workshop: "Instabilities and Structures in Proto-Planetary disks" = | {{attachment:Logo-ISPP-3.png}} = Instabilities and Structures in Proto-Planetary disks = ---- {{attachment:Univ_Provence_logo.jpg||height="50px",width="50px"}} [[Image:Logo-LAM.jpg|thumb|upright=1.2]] ---- ==== Meeting ==== * ''' Dates: 17th - 20th september 2012 ''' ## * ''' Location: Salle de l'Académie - [[http://marseille.cityseekr.com/des-accoules-church/tourist-attractions-sightseeing/venue/73217#|Les Accoules]] - [[http://en.wikipedia.org/wiki/Marseille|Marseille]] - France ''' ## * '''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. ==== Location ==== |
Instabilities and Structures in Proto-Planetary disks
Meeting
Dates: 17th - 20th september 2012
Location: Salle de l'Académie - Les Accoules - Marseille - France
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.