  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
($\lambda_{\rm in}$) and the energy (${\cal E}_{\rm in}$) at the inner sonic
point ($x_{\rm in}$), 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 ($R_{\dot{m}}^{\rm max}$) in terms of
viscosity parameter ($\alpha$) as well as black hole spin ($a_k$) and obtain
the limiting range as $3\% \le R_{\dot{m}}^{\rm max} \le 19\%$. Moreover, we
calculate the viable range of $\alpha$ that admits the coupled inflow-outflow
solutions and find that $\alpha \lesssim 0.25$ for $R_{\dot m} \ne 0$. 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 $a_k \ge 0.57$.
