Observations of the hot gas that surrounds Sgr A* and a few other nearby galactic nuclei imply that the mean free paths of electrons and protons are comparable to the gas capture radius. Hot accretion flows therefore likely proceed under weak collision conditions. As a result, thermal conduction by ions has a considerable contribution to the transfer of the realized heat in accretion mechanisms. We study a two-dimensional advective accretion disc bathed in the poloidal magnetic field of a central accretor in the presence of thermal conduction. We find self-similar solutions for an axisymmetric, rotating, steady, viscous-resistive, magnetized accretion flow. The dominant mechanism of energy dissipation is assumed to be turbulent viscosity and magnetic diffusivity due to the magnetic field of the central accretor. We show that the global structure of advection-dominated accretion flows (ADAFs) is sensitive to viscosity, advection and thermal conduction parameters. We discuss how the radial flow, angular velocity and density of accretion flows may vary with the advection, thermal conduction and viscous parameters.

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