Bounds on the Lyapunov Exponent of Circular Null Orbits in $n$-Dimensional Black-Hole Spacetimes
Unstable circular null orbits provide a geometric bridge between black-hole optics, photon rings, strong gravitational lensing, and the eikonal sector of quasinormal ringing. In four-dimensional Einstein gravity, the instability rate of such orbits, measured by the Lyapunov exponent $\lambda$, obeys model-independent upper bounds when the matter sector satisfies standard energy conditions. We extend this analysis to static, spherically symmetric, asymptotically flat black holes in arbitrary dimensional Einstein gravity, allowing for an anisotropic matter distribution. We show that, under the tangential null energy condition, the Lyapunov exponent admits a dimension-dependent upper bound in terms of the generalized surface gravity $\kappa (r)$ and the metric function $\mu(r)$, both evaluated at the photon sphere $r =r_\gamma$. For $n$- dimensional black hole spacetime, the bound is $\lambda\leq\sqrt{n-3}\, {\kappa_\gamma}/{\sqrt{\mu_\gamma}}$. Related bounds are derived in terms of the critical impact parameter (shadow radius), the orbital frequency, a local acceleration scale, and eikonal quasinormal-mode damping. All principal inequalities reduce to the known four-dimensional results for $n=4$. Also, the bounds involving the critical impact parameter and orbital frequency are saturated by the Schwarzschild-Tangherlini vacuum solution. The results provide a compact set of consistency conditions linking the dimensionality of spacetime to the instability of photon trapping in Einstein gravity.