We study the properties of the dissipative accretion flow around rotating black holes in presence of mass loss .
We obtain the complete set of global inflow-outflow solutions in the steady state by solving the underlying conservation equations self-consistently .
We observe that global inflow-outflow solutions are not the isolated solution , instead such solutions are possible for wide range of inflow parameters .
Accordingly , we identify the boundary of the parameter space for outflows , spanned by the angular momentum ( \lambda _ { in } ) and the energy ( { \cal E } _ { in } ) at the inner sonic point ( x _ { in } ) , as function of the dissipation parameters and find that parameter space gradually shrinks with the increase of dissipation rates .
Further , we examine the properties of the outflow rate R _ { \dot { m } } ( defined as the ratio of outflow to inflow mass flux ) and ascertain that dissipative processes play the decisive role in determining the outflow rates .
We calculate the limits on the maximum outflow rate ( R _ { \dot { m } } ^ { max } ) in terms of viscosity parameter ( \alpha ) as well as black hole spin ( a _ { k } ) and obtain the limiting range as 3 \% \leq R _ { \dot { m } } ^ { max } \leq 19 \% .
Moreover , we calculate the viable range of \alpha that admits the coupled inflow-outflow solutions and find that \alpha \lesssim 0.25 for R _ { \dot { m } } \neq 0 .
Finally , we discuss the observational implication of our formalism to infer the spin of the black holes .
Towards this , considering the highest observed QPO frequency of black hole source GRO J1655-40 ( \sim 450 Hz ) , we constrain the spin value of the source as a _ { k } \geq 0.57 .