The structure of self-gravitating accretion disks is investigated. In order to describe this, we establish the quantitative changes in the θ direction by solving a set of ordinary differential equations in the spherical coordinates (r, θ, φ). The use of a spherical coordinate system causes a positive radial velocity to indicate the presence of an outflow region and a negative radial velocity to indicate an inflow region. In order to discuss the regions of inflow and outflow of self-gravitating disks, we assume that the disk is axisymmetric, that is ∂/∂ϕ = 0. We also consider the disk to be steady and uniform. We use self-similar solution in the radial direction. By inserting the advection factor in the energy equation, we can distinguish standard disks from inefficient irradiation accretion disks. The effect of self-gravity of the disk is considered both in the radial and angular direction in the momentum equation. After solving the equations, the results show that the self-gravity decreases the disk’s inflow/outflow region which is observed both in gas-pressure-dominated and radiation-pressure-dominated standard accretion disks. The self-gravity can affect the angular and vertical structure and thickness of the disks. The results show that by increasing the mass of the disk, the thickness of the disk decreases. In radial direction, the self-gravity force reduces the outflow region of the disk.
