Differences between revisions 3 and 85 (spanning 82 versions)
|
Size: 1148
Comment:
|
Size: 968
Comment:
|
| Deletions are marked like this. | Additions are marked like this. |
| Line 1: | Line 1: |
| = "Instabilities and Structures in Proto-Planetary disks" = | = Instabilities and Structures in Proto-Planetary disks = ---- ==== Dates: ==== .## ''' 17th - 20th september 2012 ''' |
| Line 3: | Line 6: |
| ## ==== [[Location|Location]]: Les Accoules - Marseille - France ==== |
|
| Line 4: | Line 9: |
| Dates: 17-20 september 2012. | ## * '''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. |
| Line 6: | Line 16: |
| Location: The meeting will take place in the historical heart of the city, in the ancient room of the "Academie des Sciences, art et belles lettres" (Preau des Accoules). This is close to the "Old Harbour" a pleasant place in Marseille in september. Rationale: The meeting will address the evolution of the protoplanetary disks at the decoupling stage. The goal is to focus on, (i) 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) (ii) their lifetime and evolution (stability, migration, collisions ....), (iii) 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. |
. 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. |
Instabilities and Structures in Proto-Planetary disks
Dates:
## 17th - 20th september 2012
[[Location|Location]]: 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.