  Hydrodynamics and magnetohydrodynamic simulations of hot accretion flow have
indicated that there is an inward decreasing of mass accretion rate with
decreasing radius. Consequently, we have a flatter density profile ($\rho
\propto r^{-p}$ with $p\propto 1.5-s$ in the case of $\dot{M}\propto r^{s}$, $0
\leq s<1$) compared to the case of a constant accretion rate (($\rho \propto
r^{-\frac{3}{2}}$). In order to describe this behavior two models have been
proposed: inflow-outflow solution and convection-dominated accretion flows. We
have studied the properties of a hot accretion flow in the presence of
convection, large scale magnetic field and outflow. We consider an axisymmetric
viscous flow in the steady state. We used the self-similar solutions to solve
the 1.5 dimensional inflow-outflow equations. We have assumed that the
convection as a free parameter in our model for simplicity. We have considered
two components of magnetic field (toroidal and vertical) in this paper. We have
shown that the strong convection makes the inflow accretes and rotates slower
while it becomes hotter and thicker. We have found that the thickness of the
disc deviates from non-convective solutions obviously. We have represented that
two components of magnetic field have the opposite effects on the thickness of
the disc and similar effects on the radial and angular velocities of the flow.
