Summary: For a steady, thin Keplerian disc around a Kerr black hole, the analytical expressions for the energy fluxes released by the Kerr disc are derived by using the conservation laws of angular momentum and energy in the case of the coexistence of the jet and the Kerr disc, when the angular momentum loss owing to the jet is taken into account. It is shown that the energy flux \(F\) becomes lower, and increases monotonically with the increasing BH spin for a given accretion rate. In addition, we find that the energy flux \(F\) in the case of \(a_*= 0.998\) is about three orders of magnitude greater than its value in the case of \(a_*=0\). The results are consistent with the observations of astronomy.