Rotating kiselev black holes in <i>f</i>(<i>R</i>, <i>T</i>) gravity

Abstract Exact solutions describing rotating black holes can provide significant opportunities for testing modified theories of gravity, which are motivated by the challenges posed by dark energy and dark matter. Starting with a spherical Kiselev black hole as a seed metric, we construct rotating Kiselev black holes within the f ( R , T ) gravity framework using the revised Newman-Janis algorithmthe f ( R , T ) gravity-motivated rotating Kiselev black holes (FRKBH) with additional parameter quintessence parameter ω and state parameter γ , apart from mass M and spin a , which encompasses, as exceptional cases, Kerr ( K = 0) and effective Kerr-Newman ( K = Q 2 ) black holes. These solutions give rise to distinct classes of black holes surrounded by fluids while considering specific values of the w for viable choices for the f ( R , T ) function. From the parameter space or domain of existence of black holes defined by a and γ for FKRBH, we discover that when a 1 &lt; a &lt; a 2 , there is a critical value γ = γ E which corresponds to extreme value black holes portrayed by degenerate horizons. When a &lt; a 1 ( a &gt; a 2 ), we encounter two distinct critical values γ = γ E 1 , γ E 2 with γ E 1 &gt; γ E 2 (or γ = γ E 3 , γ E 4 with γ E 3 &gt; γ E 4 ). We discuss the horizon and global structure of FKRBH spacetimes and examine their dependence on parameters w and γ . This exploration is motivated by the remarkable effects of f ( R , T ) gravity, which gives rise to diverse and intricate spacetime structures within the domain where black holes exist.

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