The goal of this thesis is to understand the black hole accretion process, outflows and jets, and predict its observational properties. In the study of accretion disc the highly non-linear process involves a transport of angular momentum by turbulent viscosity process and dissipation in the disc by various dissipative process. The disc in a full general relativistic regime is a very hard to study analytically. So here firstly, we have study analytically hydrodynamic disc with using pseudo-Newtonian geometry around compact objects then using full general relativistic approach.

Our accretion solutions are stationary, axisymmetric without or with turbulent viscosity in the disc around non-rotating black holes. We have developed all type of possible accretion solutions in a self-consistent manner for non-dissipative or dissipative process in the disc. We have mainly focused on shock disc solutions and jets solutions by assuming jets flow geometry around BH with their corresponding disc luminosities. From this study We want to relate the four features of a black hole observations, which are the disc luminosity, Quasi-periodic Oscillations (QPOs), spectral states of the disc and emitted jets from the disc and try to connect all these observed features each other with shocked accretion disc around black holes.