  We present the global solutions of low angular momentum, inviscid, advective
accretion flow around Kerr-Taub-NUT (KTN) black hole in presence and absence of
shock waves. These solutions are obtained by solving the governing equations
that describe the relativistic accretion flow in KTN spacetime which is
characterized by the Kerr parameter ($a_{\rm k}$) and NUT parameter ($n$).
During accretion, rotating flow experiences centrifugal barrier that eventually
triggers the discontinuous shock transition provided the relativistic shock
conditions are satisfied. In reality, the viability of shocked accretion
solution appears more generic over the shock free solution as the former
possesses high entropy content at the inner edge of the disc. Due to shock
compression, the post-shock flow (equivalently post-shock corona, hereafter
PSC) becomes hot and dense, and therefore, can produce high energy radiations
after reprocessing the soft photons from the pre-shock flow via inverse
Comptonization. In general, PSC is characterized by the shock properties,
namely shock location ($r_s$), compression ratio ($R$) and shock strength
($S$), and we examine their dependencies on the energy (${\cal E}$) and angular
momentum ($\lambda$) of the flow as well as black hole parameters. We identify
the effective domain of the parameter space in $\lambda-{\cal E}$ plane for
shock and observe that shock continues to form for wide range of flow
parameters. We also find that $a_{\rm k}$ and $n$ act oppositely in determining
the shock properties and shock parameter space. Finally, we calculate the disc
luminosity ($L$) considering free-free emissions and observe that accretion
flows containing shocks are more luminous compared to the shock free solutions.
