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We present the global solutions of low angular momentum, inviscid, advectiveaccretion flow around Kerr-Taub-NUT (KTN) black hole in presence and absence ofshock waves. These solutions are obtained by solving the governing equationsthat describe the relativistic accretion flow in KTN spacetime which ischaracterized by the Kerr parameter ($a_{\rm k}$) and NUT parameter ($n$).During accretion, rotating flow experiences centrifugal barrier that eventuallytriggers the discontinuous shock transition provided the relativistic shockconditions are satisfied. In reality, the viability of shocked accretionsolution appears more generic over the shock free solution as the formerpossesses high entropy content at the inner edge of the disc. Due to shockcompression, the post-shock flow (equivalently post-shock corona, hereafterPSC) becomes hot and dense, and therefore, can produce high energy radiationsafter reprocessing the soft photons from the pre-shock flow via inverseComptonization. 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 angularmomentum ($\lambda$) of the flow as well as black hole parameters. We identifythe effective domain of the parameter space in $\lambda-{\cal E}$ plane forshock and observe that shock continues to form for wide range of flowparameters. We also find that $a_{\rm k}$ and $n$ act oppositely in determiningthe shock properties and shock parameter space. Finally, we calculate the discluminosity ($L$) considering free-free emissions and observe that accretionflows containing shocks are more luminous compared to the shock free solutions.

Study of relativistic accretion flow around KTN black hole with shocks