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MRI-driven angular momentum transport in protoplanetary disks

Published online by Cambridge University Press:  27 September 2013

S. Fromang
S. Fromang*
Affiliation:
Laboratoire AIM, CEA/DSM-CNRS-Université Paris Diderot, IRFU/Service d'Astrophysique, CEA–Saclay, 91191 Gif-sur-Yvette, France
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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.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 62: Role and Mechanisms of Angular Momentum Transport During the Formation and Early Evolution of Stars Evry Schatzman School 2012 , 2013 , pp. 95 - 142
Copyright
© EAS, EDP Sciences, 2013

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