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We study the global accretion-ejection solutions around a rotating black holeconsidering three widely accepted pseudo-Kerr potentials that satisfactorilymimic the space-time geometry of rotating black holes. We find that all thepseudo potentials provide standing shock solutions for large range of flowparameters. We identify the effective region of the shock parameter spacespanned by energy ($\mathcal{E}_{\text{in}}$) and angular momentum($\lambda_{\text{in}}$) measured at the inner critical point ($x_{\text{in}}$)and find that the possibility of shock formation becomes feeble when theviscosity parameter ($\alpha$) is increased. In addition, we find that shockparameter space also depends on the adiabatic index ($\gamma$) of the flow andthe shock formation continues to take place for a wide range of $\gamma$ as$1.5 \le \gamma \le 4/3$. For all the pseudo potentials, we calculate thecritical viscosity parameter ($\alpha_{\text{shock}}^{\text{cri}}$) beyondwhich standing shock ceases to exist and compare them as function of black holespin ($a_k$). We observe that all the pseudo potentials under consideration arequalitatively similar as far as the standing shocks are concerned, however,they differ both qualitatively and quantitatively from each other for rapidlyrotating black holes. Further, we compute the mass loss from the disc using allthree pseudo potentials and find that the maximum mass outflow rate ($R^{\rmmax}_{{\dot m}}$) weakly depends on the black hole spin. To validate our model,we calculate the maximum jet kinetic power using the accretion-ejectionformalism and compare it with the radio jet power of low-hard state of theblack hole X-ray binaries (hereafter XRBs). The outcome of our results indicatethat XRBs along the `outliers' track might be rapidly rotating.

Accretion-ejection in rotating black holes: a model for `outliers' track of radio-X-ray correlation in X-ray binaries