MRI-driven angular momentum transport in protoplanetary disks
arXiv:1305.3416 · doi:10.1051/eas/1362004
Abstract
Angular momentum transport in accretion disk has been the focus of intense research in theoretical astrophysics for many decades. In the past twenty years, MHD turbulence driven by the magnetorotational instability has emerged as an efficient mechanism to achieve that goal. Yet, many questions and uncertainties remain, among which the saturation level of the turbulence. The consequences of the magnetorotational instability for planet formation models are still being investigated. This lecture, given in September 2012 at the school "Role and mechanisms of angular momentum transport in the formation and early evolution of stars" in Aussois (France), aims at introducing the historical developments, current status and outstanding questions related to the magnetorotational instability that are currently at the forefront of academic research.
51 pages, 16 figures, to appear in the proceedings of the Evry Schatzman School 2012 of PNPS and CNRS/INSU on the "Role and mechanisms of angular momentum transport during the formation and early evolution of stars", Eds. P.Hennebelle & C.Charbonnel
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Cited by in corpus (6)
- Modelling MHD accretion-ejection - from the launching area to propagation scales
- Modelling MHD accretion-ejection - episodic ejections of jets triggered by a mean-field disk dynamo
- Angular momentum transport and large eddy simulations in magnetorotational turbulence: the small Pm limit
- 3D evolution of magnetic fields in a differentially rotating stellar radiative zone
- Jets from accretion disk dynamos: consistent quenching modes for dynamo and resistivity
- Quasi-two-dimensional nonlinear evolution of helical magnetorotational instability in a magnetized Taylor-Couette flow