  We study the relativistic, inviscid, advective accretion flow around the
black holes and investigate a key feature of the accretion flow, namely the
shock waves. We observe that the shock-induced accretion solutions are
prevalent and such solutions are commonly obtained for a wide range of the flow
parameters, such as energy (${\cal E}$) and angular momentum ($\lambda$),
around the black holes of spin value $0\le a_{\rm k} < 1$. When the shock is
dissipative in nature, a part of the accretion energy is released through the
upper and lower surfaces of the disc at the location of the shock transition.
We find that the maximum accretion energies that can be extracted at the
dissipative shock ($\Delta{\cal E}^{\rm max}$) are $\sim 1\%$ and $\sim 4.4\%$
for Schwarzschild black holes ($a_{\rm k}\rightarrow 0$) and Kerr black holes
($a_{\rm k}\rightarrow 1$), respectively. Using $\Delta{\cal E}^{\rm max}$, we
compute the loss of kinetic power (equivalently shock luminosity, $L_{\rm
shock}$) that is enabled to comply with the energy budget for generating
jets/outflows from the jet base ($i.e.$, post-shock flow). We compare $L_{\rm
shock}$ with the observed core radio luminosity ($L_R$) of black hole sources
for a wide mass range spanning $10$ orders of magnitude with sub-Eddington
accretion rate and perceive that the present formalism seems to be potentially
viable to account $L_R$ of $16$ Galactic black hole X-ray binaries (BH-XRBs)
and $2176$ active galactic nuclei (AGNs). We further aim to address the core
radio luminosity of intermediate-mass black hole (IMBH) sources and indicate
that the present model formalism perhaps adequate to explain core radio
emission of IMBH sources in the sub-Eddington accretion limit.
