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| = Workshop: "Instabilities and Structures in Proto-Planetary disks" = | {{attachment:Logo-ISPP-3.png}} = Instabilities and Structures in Proto-Planetary disks = ---- [[http://http://lam.oamp.fr/index.php|{{attachment:Logo-LAM.jpg||width=150}}|target="LAM/OAMP"]] [[http://www.univ-provence.fr/public_html/univ-provence/index.php?pages=article&id=2144&idnum=2405&m=872|{{attachment:Univ_Provence_logo.jpg||width=50}}|target="Provence University"]] [[http://www.cnrs.fr/index.php|{{attachment:Logo-CNRS.gif||width=100}}|target="CNRS"]] [[http://http://www.regionpaca.fr/en.html|{{attachment:logo-paca.jpg||width=150}}|target="Region PACA"]] ---- ==== 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.