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| Paper: |
The Role of Physical Viscosity on Accretion Disc Dynamics in Close Binaries and AGN |
| Volume: |
385, Numerical Modeling of Space Plasma Flows: Astronum-2007 |
| Page: |
115 |
| Authors: |
Lanzafame, G. |
| Abstract: |
The role of turbulent physical viscosity is here considered as far as an accretion disc is concerned both in close binaries (CB) and around massive black holes in active galactic nuclei (AGN). The study has been performed via SPH simulations of disc models. Physical viscosity has been considered according to the Shakura and Sunjaev α prescription. Results show that physical viscosity supports and favours accretion disc formation in low compressibility models. Spiral shocks in the radial flux develop only in some high compressibility models. Physical viscosity efficiently supports mass, angular momentum and heat radial transport towards the compact primary star as well as the radial disc spread. Results show that compressibility-viscosity domains exist, where turbulent physical viscosity supports the accretion disc formation. A role also played by the injection kinematics at the inner Lagrangian point L1 is also found. A grid of physically viscous 3D SPH, axially symmetric, accretion disc simulations around black holes (BH) in AGN, have also been performed, paying also attention to the role of the specific angular momentum λ as an initial boundary condition at the disc outer edge. A shock front usually develops, according to assigned outer edge initial and boundary conditions, mainly due to the centrifugal barrier. Pairs of (λ, α) values exist, determining radial periodical oscillations in the shock front. Periodical outflows can develop from the subsonic post shock region close to the BH in some cases. |
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