The correlated and coupled dynamics of accretion and outflow around black holes ( BHs ) are essentially governed by the fundamental laws of conservation as outflow extracts matter , momentum and energy from the accretion region .
Here we analyzed a robust form of 2.5-dimensional viscous , resistive , advective magnetized accretion-outflow coupling in BH systems , in the mean field magnetohydrodynamical ( MHD ) regime .
We solve the complete set of coupled MHD conservation equations self-consistently , through invoking a generalized polynomial expansion in two dimensions .
We perform a critical analysis of accretion-outflow region and provide a complete quasi-analytical family of solutions for advective flows .
We obtain the physical plausible outflow solutions at high turbulent viscosity parameter \alpha ( \raisebox { -1.72 pt } { $ \stackrel { > } { \scriptstyle \sim } $ } 0.3 ) , and at a reduced scale-height , as magnetic stresses compress or squeeze the flow region .
We found that the value of the large-scale poloidal magnetic field \bar { B } _ { P } is enhanced with increasing geometrical thickness of the accretion flow .
On the other hand differential magnetic torque ( - r ^ { 2 } \bar { B } _ { \varphi } \bar { B } _ { z } ) increases with the increase in \dot { M } . \bar { B } _ { P } , - r ^ { 2 } \bar { B } _ { \varphi } \bar { B } _ { z } as well as the plasma beta \beta _ { P } get strongly augmented with the increase in the value of \alpha , enhancing the transport of vertical flux outwards .
Our solutions indicate that magnetocentrifugal acceleration plausibly plays a dominant role in effusing out plasma from the radial accretion flow in moderately advective paradigm which are more centrifugally dominated , however in strongly advective paradigm it is likely that the thermal pressure gradient would play a more contributory role in the vertical transport of the plasma .