Magnetized, mass-loaded, rotating accretion flows

We present a semi-analytical investigation of a simple one-dimensional, ste ady-state model for a mass-loaded, rotating, magnetized, hydrodynamical flo w. Our approach is analogous to one used in early studies of magnetized win ds. The model represents the infall towards a central point mass of the gas generated in a cluster of stars surrounding it, as is likely to occur in s ome active nuclei and starburst galaxies. We describe the properties of the different classes of infall solutions. We find that the flow becomes faste r than the fast-mode speed, and hence decoupled from the centre, only for a limited range of parameter values, and when magnetic stresses are ineffect ive. Such flow is slowed as it approaches a centrifugal barrier, implying t he existence of an accretion disc. When the flow does not become super-fast and the magnetic torque is insufficient, no steady solution extending inwa rd to the centre exists. Finally, with a larger magnetic torque, solutions representing steady sub-Alfvenic flows are found, which can resemble spheri cal hydrodynamical infall. Such solutions, if applicable, would imply that rotation is not important and that any accretion disc formed would be of ve ry limited size.