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要旨:
We consider the specific case of disc accretion for low viscosity and high electric conductivity
of plasma. The key component in this model is magnetized wind outflowing from the accretion
disc. This wind effectively carries away angular momentum of the accreting matter. Assuming
variable magnetic field polarity in the disc (to avoid magnetic flux and energy accumulation at
the gravitational center), this leads to radiatively inefficient accretion of the disc matter onto the
gravitational center. Interestingly, that in this framework, the basic properties of the outflow
(as well as angular momentum and energy flux per particle in the outflow) do not depend on
the accretion disc structure. The obtained self-similar solutions prove the existence of such an
accreting regime. The outflow predominantly occurs from the very central part of the disc. The
accretion/outflow mechanism provides transformation of the gravitational energy of the accreted
matter into the energy of the outflowing wind with efficiency close to 100%. The flow velocity
can essentially exceed the Kepler velocity at the site of the wind launch
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