The accretion torus which is a disk-like luminous structure of gaseous substrate is known to be orbiting supermassive black holes that reside at the center of the galaxies. As these structures serve as perfect probe objects for astrophysical black holes in the strong-gravity regime, one expects the black hole can significantly influence the morphology of the torus in presence of non-minimal interactions of the gravitational field of the black hole with the disk fluid. In this talk, I present such an interesting scenario when a torus endowed with macroscopic spin fluid is located in stationary axially symmetric spacetime. Given that macroscopic spin of the disk fluid gets non-minimally coupled with the curvature tensor, it is found that stationary equilibrium solutions demonstrate explicit modification of torus morphology due to spin-curvature coupling respectively in Schwarzschild and in Kerr spacetime. Lastly, an estimation of spin is proposed for such an accretion disk composed of spin 1/2 particles.