We consider an extreme case of disc accretion onto a gravitating centre when the viscosity in the disc is negligible .
The angular momentum and the rotational energy of the accreted matter is carried out by a magnetized wind outflowing from the disc .
The outflow of matter from the disc occurs due to the Blandford & Payne ( 1982 ) centrifugal mechanism .
The disc is assumed to be cold .
Accretion and outflow are connected by the conservation of the energy , mass and the angular momentum .
The basic properties of the outflow , angular momentum flux and energy flux per particle in the wind , do not depend on the details of the structure of the accretion disc .
In the case of selfsimilar accretion/outflow , the dependence of the rate of accretion \dot { M } in the disc depends on the disc radius r on the law \dot { M } \sim r ^ { { 1 \over 2 ( \alpha ^ { 2 } -1 ) } } , where \alpha is a dimensionless Alfvenic radius .
In the case of \alpha \gg 1 , the accretion in the disc is provided by very weak matter outflow from the disc and the outflow predominantly occurs from the very central part of the disc .
The solution obtained in the work provides mechanism which transforms the gravitational energy of the accreted matter into the energy of the outflowing wind with efficiency close to 100 \% .
The final velocity can essentially exceed Kepler velocity at the site of the wind launch .
This mechanism allows us to understand the nature of the astrophysical objects with low luminosity discs and energetic jet-like outflows .