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

Abstract

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

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Cited by in corpus (4)

• The Role of Outflow Feedback on Accretion of Compact Objects in Accretion Disk of Active Galactic Nuclei
• Global Transonic Solution of Hot Accretion Flow with Thermal Conduction
• Self-similar structure of resistive ADAFs with outflow and large-scale magnetic field
• Resistive Hot Accretion Flows with Anisotropic Pressure