  We examine the effects of a global magnetic field and outflow on radiatively
inefficient accretion flow (RIAF) in the presence of magnetic resistivity. We
find a self-similar solutions for the height integrated equations that govern
the behavior of the flow. We use the mixing length mechanism for studying the
convection parameter. We adopt a radius dependent mass accretion rate as
$\dot{M}=\dot{M}_{out}{(\frac{r}{r_{out}})^{s}}$ with $s> 0$ to investigate the
influence of outflow on the structure of inflow where $s$ is a constant and
indication the effect of wind. Also, we have studied the radiation spectrum and
temperature of CDAFs. The thermal bermsstrahlung emission as a radiation
mechanism is taken into account for calculating the spectra emitted by the
CDAFs. The energy that powers bremsstrahlung emission at large radii is
provided by convective transport from small radii and viscous and resistivity
dissipation. Our results indicate that the disc rotates slower and accretes
faster, it becomes hotter and thicker for stronger wind. By increasing all
component of magnetic field, the disc rotates faster and accretes slower while
it becomes hotter and thicker. We show that the outflow parameter and all
component of magnetic field have the same effects on the luminosity of the
disc. We compare the dynamical structure of the disc in two different solutions
(with and without resistivity parameter). We show that only the radial infall
velocity and the surface density could changed by resistivity parameter
obviously. Increasing the effect of wind increases the disc's temperature and
luminosity of the disc. The effect of magnetic field is similar to the effect
of wind in the disc's temperature and luminosity of the disc, but the influence
of resistivity on the observational properties is not evident.
