The Effect of Toroidal Magnetic Field on Thickness of a Viscose-Resistive Hot Accreting Flow

Abstract

By taking into account the effect of toroidal magnetic field and its correspond heating, we determine the thickness of advection-dominated accretion flows. We consider an axisymetric, rotating, steady viscous-resistive, 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 self-similar assumption in the radial direction to obtain the dynamical quantities, that is, radial, azimuthal, sound and Alfv\' en 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 non-magnetic case, in general the disc half-thikness, $\Delta \theta$, 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, ${\beta }_0$, showing the magnetic field strength at the equatorial plane, decreases $\Delta \theta$. The other one, ${\eta }_0$ is the magnetic resistivity parameter and when it increases, $\Delta \theta$ increases, too.

To appear in MNRAS

References in corpus (3)

• Advection/Diffusion of Large-Scale B-Field in Accretion Disks
• Hydrodynamical wind on a magnetized ADAF with thermal conduction
• Structure of Advection-Dominated Accretion Disks with Outflows: Role of Toroidal Magnetic Field

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• Standing Shocks in Magnetized Dissipative Accretion Flow around Black Holes
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• Accretion flows with comparable radiation and gas pressures
• Anchoring polar magnetic field in a stationary thick accretion disk
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• Fourier analysis of advection-dominated accretion flows