Viscosity-Driven Winds from Magnetized Accretion Disks
arXiv:astro-ph/0306328 · doi:10.1086/376402
Abstract
We present an analytic model in which an inefficiently radiating accretion disk drives upward wind from its surfaces. The accretion process is controlled simultaneously by a global magnetic field penetrating the disk and by a viscosity of the accreting plasma. It is shown that energy is transported radially outward within the accreting flow, associated with the viscous angular-momentum transport in the same direction, and that this addition of energy from the inner part to the disk part makes the latter possible to drive an upward wind. The parameter that specifies the strength of a wind is determined uniquely in terms of a naturally introduced viscosity parameter.
accepted for publication in ApJ
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