Turbulent, Magnetized, M R I - driven Accretion Disks: Beyond The α-disk Models

Details Turbulent, Magnetized, M R I - driven Accretion Disks: Beyond The α-disk Models Turbulent, Magnetized, M R I - driven Accretion Disks: Beyond The α-disk Models

Sep 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006head....9.0204p&link_type=abstract

American Astronomical Society, HEAD meeting #9, #2.04; Bulletin of the American Astronomical Society, Vol. 38, p.344

Physics

Scientific paper

The last decade has witnessed significant advances in numerical
simulations of turbulent, magnetized accretion disks. However, because of
the large temporal and spatial dynamical ranges involved, the study of the
long-term evolution of the accretion flows and of the accreting central
objects will remain beyond reach in the near future. In order to address,
some of the long-standing problems in accretion physics, such as the
growth of supermassive black holes, the stability of accretion disks, and
the spin-orbit alignment of accreting compact objects in binaries, it is
necessary for us to follow a different approach. In this talk, I will
present the first dynamical, mean-field model for angular momentum
transport in thin accretion disks that is physically motivated,
incorporates the MRI as the main driver of the MHD turbulence, and
reproduces the results of local three-dimensional numerical simulations.
The model possesses several appealing characteristics: it generates
turbulence only where the disk is MRI-unstable and does not suffer from
causality problems across sonic points. Moreover, because it incorporates
explicitly the advection of the turbulent stresses, it naturally leads to
non-vanishing torques inside the marginally stable orbit, in agreement
with global numerical simulations. I will discuss the implications of the
model for the global structure of accretion disks and for the
observational signatures of the marginally stable orbit.

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