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We study the properties of a low-angular momentum, inviscid, advectiveaccretion flow in a deformed Kerr spacetime under the framework of generaltheory of relativity. We solve the governing equations that describe the flowmotion in terms of input parameters, namely energy ($E$), angular momentum($\lambda$), spin ($a_{\rm k}$) and deformation parameter ($\varepsilon$),respectively. We find that global transonic accretion solutions continue toexist in non-Kerr spacetime. Depending on the input parameters, accretion flowis seen to experience shock transition and we find that shocked inducedaccretion solutions are available for a wide range of the parameter space in$\lambda-E$ plane. We examine the modification of the shock parameter spacewith $\varepsilon$, and find that as $\varepsilon$ is increased, the effectiveregion of the parameter space is reduced, and gradually shifted towards thehigher $\lambda$ and lower $E$ domain. In addition, for the first time in theliterature, we notice that accretion flow having zero angular momentum admitsshock transition when spacetime deformation is significantly large.Interestingly, beyond a critical limit of $\varepsilon^{\rm max}$, the natureof the central object alters from black hole (BH) to naked singularity (NS) andwe identify $\varepsilon^{\rm max}$ as function of $a_{\rm k}$. Further, weexamine the accretion solutions and its properties around the naked singularityas well. Finally, we indicate the implications of the present formalism in thecontext of astrophysical applications.

Properties of accretion flow in deformed Kerr spacetime