2018ApJ...865...93G

In this work, we study the vertical structure of a hot accretion flow by taking into account radial transportation of angular momentum and energy due to the presence of turbulence, convection, and outflow. We write the hydrodynamics equations in the spherical coordinates, and, based on the assumptions of axisymmetric and steady state, we simplify the basic equations. Employing self-similar solutions in the radial direction and finding proper boundary conditions, we solve the ordinary differential equations with respect to the polar angle. Considering the meridional component of the velocity field, we find inflow-outflow solutions. In order to formulate the convection term, we introduce two parameters, i.e., α_c and g as free parameters. The first one is called the convection parameter and the greater value of it makes the convection more effective in changing the flow dynamics. The second one, g, varies between zero and unity (where g = 1 implies that the convection behaves similarly to the turbulence viscosity and g = 0 means the convection behaves in the opposite direction of viscosity). Our results show that the accretion rate decreases with greater α_c and it makes the disk warmer and intensifies the outflows from the disk's surface. On the other hand, the g parameter affects the flow in an opposite manner compared to the convection parameter and makes the disk rotate and accrete faster.