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Theory of Turbulent Accretion Disks

Published online by Cambridge University Press:  25 September 2002

J. Bouvier ,
J.-P. Zahn  and
C. E.J.M.L.J. Terquem
C. E.J.M.L.J. Terquem*
Affiliation:
Institut d'Astrophysique de Paris, France Université Denis Diderot-Paris VII, France
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Abstract

In low-mass disks, turbulent torques are probably the most importantway of redistributing angular momentum. Here we present the theory ofturbulent accretion disks. We show the molecular viscosity is far toosmall to account for the evolutionary timescale of disks, and wedescribe how turbulence may result in enhanced transport of (angular)momentum. We then turn to the magnetorotational instability, whichthus far is the only mechanism that has been shown to initiate andsustain turbulence in disks. Finally, we present both the basis andthe structure of α disk models.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 3: Star Formation and the Physics of Young Stars: Summer school on Stellar Physics X , 2002 , pp. 203 - 228
Copyright
© EAS, EDP Sciences, 2002

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