Steady Models of Optically Thin, Magnetically Supported Black Hole Accretion Disks

We obtained steady solutions of optically thin, single-temperature, magnetized black hole accretion disks, assuming thermal bremsstrahlung cooling. Based on the results of 3D MHD simulations of accretion disks, we assumed that the magnetic fields inside the disk are turbulent and dominated by an azimuthal component. We decomposed the magnetic fields into an azimuthally averaged mean field and fluctuating fields. We also assumed that the azimuthally averaged Maxwel ls tress i sp roportional to the total pressure. The radial advection rate of the azimuthal magnetic flux, P Φ ,i s prescribed as being proportional to $ � � ,w here$ is the radial coordinate