[Modèles expérimentaux des disques d’accrétion MHD]
Cet article de revue résume deux décennies de recherche en laboratoire visant à comprendre la dynamique des disques astrophysiques, en mettant particulièrement l’accent sur les expériences magnétohydrodynamiques impliquant des métaux liquides et des plasmas. Tout d’abord, les expériences de Taylor–Couette ont démontré la génération de l’instabilité magnétorotationnelle (MRI) dans les métaux liquides, et ont mis en évidence la façon dont cette instabilité est influencée de manière critique par les conditions aux limites et la géométrie du champ magnétique appliqué. Ces expériences permettent également de mieux comprendre la transition non linéaire vers la turbulence dans les disques d’accrétion et leur lien avec d’autres instabilités dans les écoulements centrifuges stables. Une approche complémentaire, impliquant des expériences de laboratoire avec un entraînement volumique du fluide plutôt qu’avec un dispositif en rotation, permet une étude quantitative du transport du moment cinétique par la turbulence Képlèrienne. Collectivement, ces diverses études de laboratoire offrent de nouvelles contraintes sur les modèles théoriques visant à expliquer la dynamique des disques d’accrétion. Ceci est particulièrement vrai en ce qui concerne le rôle de la turbulence Képlèrienne dans les disques proto-planétaires, dont les récentes observations du télescope ALMA ont considérablement révisé les valeurs précédemment attendues pour l’amplitude des fluctuations turbulentes. Enfin, l’article aborde les questions en suspens et les perspectives futures dans la modélisation en laboratoire des disques d’accrétion.
This review article summarizes two decades of laboratory research aimed at understanding the dynamics of accretion disks, with particular emphasis on magnetohydrodynamic experiments involving liquid metals and plasmas. First, the Taylor–Couette experiments demonstrated the generation of magnetorotational instability (MRI) in liquid metals, and highlighted how this instability is critically influenced by boundary conditions and the geometry of the applied magnetic field. These experiments also highlight the nonlinear transition to turbulence in accretion disks, and their link with other MHD instabilities in centrifugally-stable flows. A complementary approach, involving laboratory experiments with volumetric fluid driving rather than rotating boundaries, enables a quantitative study of angular momentum transport by Keplerian turbulence. Collectively, these various laboratory studies offer new constraints on the theoretical models designed to explain the dynamics of accretion disks. This is particularly true with regard to the role of Keplerian turbulence in protoplanetary disks, where recent observations from the ALMA telescope have considerably revised previously expected values of the magnitude of the turbulent fluctuations. Finally, the paper discusses outstanding questions and future prospects in laboratory modeling of accretion disks.
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Mot clés : Disques d’accrétion, magnétohydrodynamique (MHD), instabilités, turbulence, écoulements, MRI
Christophe Gissinger 1
CC-BY 4.0
@article{CRPHYS_2024__25_S3_A8_0,
author = {Christophe Gissinger},
title = {Laboratory modeling of {MHD} accretion disks},
journal = {Comptes Rendus. Physique},
publisher = {Acad\'emie des sciences, Paris},
year = {2024},
doi = {10.5802/crphys.204},
language = {en},
note = {Online first},
}
Christophe Gissinger. Laboratory modeling of MHD accretion disks. Comptes Rendus. Physique, Online first (2024), pp. 1-28. doi : 10.5802/crphys.204.
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