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We present the effects of ordered large scale magnetic field on the structureof supercritical accretion flow in the presence of outflow. In the cylindricalcoordinates ($r, \varphi,z$), We write the 1.5 dimensional, the steady state($\frac{\partial}{\partial t}=0$) and axisymmetric ($\frac{\partial}{\partial\varphi}=0$) inflow-outflow equations by using the self similar solutions. Alsoa model for radiation pressure supported accretion flow threaded by bothtoroidal and vertical components of magnetic field has been formulated.  For studying the outflows, we adopt a radius dependent mass accretion rate as$\dot{M}=\dot{M}_{out}{(\frac{r}{r_{out}})^{s+\frac{1}{2}}}$ with$s=\frac{1}{2}$. Also by following the previous works, we have considered theinterchange of mass, radial and angular momentum and the energy between inflowand outflow. we have found numerically that two components of magnetic fieldhave the opposite effects on the thickness of the disc and similar effects onthe radial and angular velocities of the flow. We have found that the existenceof the toroidal component of magnetic field will lead to increasing of radialand azimuthal velocities as well as the relative thickness of the disc, whichis increased . Moreover, the thickness of the disc will decrease when thevertical component of magnetic field becomes important in magnetized flow. Thesolutions indicated that the mass inflow rate, the specific energy of outflowaffect strongly on the advection parameter.We have shown that by increasing thetwo components of magnetic field, the temperature of the accretion flow willdecrease significantly. On the other hand we have shown the bolometricluminosity of the slim discs for high values of $\dot{m} (\dot{m}>>1)$ is notsensitive to mass accretion rate and is kept constant ($L \approx 10 L_{E}$).

The influence of large scale magnetic field in the structure of supercritical accretion flow with outflow