Based on their extended radio morphologies, radio-loud (RL) active galactic nuclei (AGNs) are principally separated into two classes: the low-radio-power Fanaroff-Riley class I (FRI) and the more radio-powerful FRIIs. This FR-dichotomy has been commonly perceived to arise either (a) owing to the impact of external ambient medium on outflow/jet propagation, or (b) due to intrinsic differences in black hole (BH) properties and/or jet production mechanism. Alternatively, based on the characteristics of their optical emission-line spectra, RL population can be classified into two distinct classes, namely low- and high-excitation radio galaxies (RGs) (i.e., the LERGs and HERGs). LERGs, a majority of them harboring low-radio-power FRI-type jets, while HERGs and/or RL quasars, mostly associated with more radio powerful FRII jets, could be viewed as possible counterparts of low-hard state (LHS) BH X-ray binaries (BHXRBS), and transition state [during LHS-to-high-soft state (HSS) at hard-intermediate state] XRBs, respectively. An intriguing aspect, however being observed, is that the significant population of LERGS are found to possess FRII-type jets, while some HERGs are found to be associated with FRI-type jets. Within the paradigm, in which different faces of AGNs appear to be the broad analogues of BHXRB states, it is expected that almost all LERGs should harbor FRI-type jets, while HERGs should harbor FRII-type jets. The existence of sub-population of FRI/FRII-type jets in LERG/HERGs and the nature of connection between accretion modes and jet-morphology (FR-class) is a subject of long-standing debate, given the fact that LERGs/HERGs have distinct galactic environments, while accretion modes in AGNs are distinctly related to galactic environments. Here I attempt to address this issue from a different approach, in the context of ‘shock’ induced by galactic gravitational potential of the host elliptical galaxy on the outflowing matter, considering a five-component galactic system (SMBH + stellar + dark matter + diffuse hot gas + \(\Lambda \) ); as a first approximation, confining to the simplest scenario of wind-type outflows. For most of the relevant range of galactic mass-to-light ratio \(\left (\Upsilon _B \right )\) , shock formation occurs in the central-to-outer regions of wind-type outflows, beyond few kiloparsecs. I discuss about the plausible implication of these shocks in the context of realistic outflow/jets, and comment on the observed FR-dichotomy in the radio sources.