Abstract

We consider steady, advective, rotating, inviscid accretion disc around the spinning black holes to compute the mass outflow rate (R_ṁ ) defined as the ratio of mass flux of outflowing to the inflowing matter. Due to centrifugal barrier, accreting matter suffers discontinuous shock transition and because of shock compression, the post-shock matter becomes hot and denser than the pre-shockmatter. We call the post-shock disc as Post Shock Corona (PSC). During accretion, a part of the inflowing matter deflects as bipolar outflows due to the presence of excess thermal gradient force at PSC. We find that R_ṁ is directly correlated with the spin of the black hole (a_k) for the same set of inflow parameter, namely specific energy (ε) and specific angular momentum (λ). We observe that the maximum outflow rate(R^max_ṁ) weakly depends on spin (a_k) that lies in the range ∼ 17% - 18% of the inflow rate.