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Paper IPM / Astronomy / 13061  


Abstract:  
By taking into account the effect of toroidal magnetic field and its correspond heating, we determine the thickness of advectiondominated accretion flows. We consider an axisymetric, rotating, steady viscousresistive, magnetized accretion flow under an advection dominated stage. The dominant mechanism of energy dissipation is assumed to be turbulence viscosity and magnetic diffusivity. We adopt a selfsimilar assumption in the radial direction to obtain the dynamical quantities, that is, radial, azimuthal, sound and Alfvén velocities. Our results show the vertical component of magnetic force acts in the opposite direction of gravity and compresses the disc, thus compared with the nonmagnetic case, in general the disc halfthikness, ∆θ, significantly is reduced. On the other hand, two parameters, appearing due to action of magnetic field and reaction of the flow, affect the disc thickness. The first one , β_{0}, showing the magnetic field strength at the equatorial plane, decreases ∆θ. The other one, η_{0} is the magnetic resistivity parameter and when it increases, ∆θ increases, too.
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