Accueil > Séminaires d’Astrophysique > MHD turbulence in protoplanetary disks, what can and can’t be learned from numerical simulations

 

MHD turbulence in protoplanetary disks, what can and can’t be learned from numerical simulations

Sébastien Fromang (CEA)

Par Stephane Charpinet - 10/03/2009

 

Séminaires d’Astrophysique

de l’Observatoire Midi-Pyrénées


Séminaire de

Sébastien FROMANG

(CEA)

Jeudi 12 Mars 2009 à 11h

OMP, salle Coriolis


MHD turbulence in protoplanetary disks, what can and can’t be learned from numerical simulations

In accretion disks, angular momentum has to be transported outward for matter to be accreted onto the central object (a young star, a compact objet or a black hole). Such a transport occurs though fully developped turbulence that is now believed to be magnetohydrodynamic in origin. Its properties (saturation, dynamo mechanism, statistical properties) and consequences are best studied using three dimensional MHD numerical simulations. Two approaches have been used in the past. The first uses local simulations that enable high resolution at the cost of realism while the second designs global simulations that are best suited to study the observational consequences and the disk large scale properties. In this talk, I will review both types of simulations and highlight their interest as well as their limitations. I will describe the recent results that have emerged in the last few years regarding the role of small scale dissipation on the saturation properties of the turbulence. Finally, I will present the consequences of MHD turbulence on the dynamics of solid particles and their possible links with past and future observations of protoplanetary disks.

 

 

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Laboratoire Astrophysique de Toulouse - Tarbes (UMR5572)

CNRS (Midi-Pyrénées)

Univ. Paul Sabatier

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