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Observational evidence and theoretical arguments postulate that outflows mayplay a significant role in the advection-dominated accretion discs (ADAFs).While the azimuthal viscosity is the main focus of most previous studies inthis context, recent studies indicated that disc structure can also be affectedby the radial viscosity. In this work, we incorporate these physicalingredients and the toroidal component of the magnetic field to explore theirroles in the steady-state structure of ADAFs. We thereby present a set ofsimilarity solutions where outflows contribute to the mass loss, angularmomentum removal, and the energy extraction. Our solutions indicate that theradial viscosity causes the disc to rotate with a slower rate, whereas theradial gas velocity increases. For strong winds, the infall velocity may be oforder the Keplerian speed if the radial viscosity is considered and thesaturated conduction parameter is high enough. We show that the strength ofmagnetic field and of wind can affect the effectiveness of radial viscosity.

The self-similar structure of advection-dominated discs with outflow and radial viscosity