Researchers have developed an equation to describe the dynamics of thin, viscous accretion disks around compact objects within the full Kerr spacetime. This formulation is valid for all values of the Kerr parameter $a$, enabling the study of both Kerr black holes ($0 < a \le 1$) and Kerr naked singularities ($a > 1$). The model incorporates exact Keplerian and Lense-Thirring precession frequencies, analytically deriving radial disk tilt profiles without recourse to slow-spin or weak-field approximations.

Numerical solutions of these equations, obtained under realistic boundary conditions, reveal significant deviations from slow-spin approximations, particularly in the inner disk where relativistic effects dominate. In the diffusive regime, the study finds that for Kerr naked singularities, the tilt profile exhibits distinct inner hump(s) near the radius where the specific angular momentum vanishes—a feature absent in Kerr black holes.

Considering the tilt in the inner disk could significantly influence the interpretation of observed X-ray spectral, timing, and polarization features. These observations are crucial for probing the strong gravity regime and inferring the spin of the central object. While the distinct hump feature alone does not uniquely distinguish Kerr black holes from Kerr naked singularities, its interpretation in conjunction with disk regime constraints may provide an observational handle on the nature of the accreting collapsed object.