Realization of the stationary integral solutions of steady-state transonic accretion flow in spherical symmetry (so called Bondi flow) is crucial, since it helps to understand accretion phenomena on various astrophysical objects. Such flows are generally studied in the literature, in general, only from astrophysical contexts. In recent years, however, attempts have been made to study accreting black hole systems as an example of autonomous dynamical systems. The fixed-point solution scheme has been borrowed from the theory of dynamical systems to study the transonic properties of accretion flow onto an astrophysical black hole, and it has been demonstrated that the nature of the phase orbit of transonic flow solutions can be understood even without constructing integral solutions. Because a large-scale astrophysical fluid flow is vulnerable to external perturbations, it is necessary to ensure that the stationary accretion solutions are stable under such perturbations. Such a task can be accomplished by adopting a time-dependent stability analysis scheme for the accretion flow, to demonstrate, under which condition the perturbation will not diverge. While performing such stability analysis, it has also been observed that a space time metric, dubbed as the sonic (or acoustic) metric can be constructed to describe the propagation of perturbations embedded within the accreting fluid. Such a sonic metric is similar in nature to certain representation of the Schwarzschild metric. Thus, the acoustic metric mimics a black hole like spacetime within the accreting fluid, and the transonic surface can be identified with a black hole like horizon. Such identification is accomplished using the theory of causal structure, by constructing Carter-Penrose diagrams. An accreting black hole system, thus, can be perceived as an classical analogue gravity model naturally found in the universe. Hence, accretion phenomena onto astrophysical black holes can be looked upon from three apparently non overlapping perspectives—astrophysical processes, theory of dynamical systems, and emergent gravity (alternatively, the analogue gravity) phenomena, respectively. The present chapter illustrates, by taking the simplest possible accretion flow model, how one can study astrophysical accretion processes from three aforementioned perspectives.