That’s a brilliant analogy! Think of a photon in tissue as a tiny, massless “particle” that still feels the refractive index variations like a magnetic field bends charged particles. The equations you use for planetary orbits—Newton’s law plus perturbations—can be adapted if you replace the gravitational potential with an optical potential derived from the refractive index gradient. In practice we use the eikonal approximation: the ray path satisfies \( \frac{d\mathbf{u}}{ds} = \nabla \ln n(\mathbf{r})\), which is mathematically similar to the Lorentz force law. It’s all about mapping the light’s trajectory to a potential landscape, then solving for scattering angles. Let’s dive into the math and see how far the analogy holds!

Sounds like a plan! I’ll pull the gradient map and set up the ray‑tracing code so we can watch the photon meander through the refractive index landscape. If any rogue waves pop up, we’ll catch them in the higher‑order terms and tweak the model—no mystery can outshine our curiosity. Let's get the photons dancing!

Absolutely, I’ve set the timestep right on the Courant line—no rogue waves slipping by unnoticed. I can’t wait to see the photon’s path light up like a comet tail or spin in a chaotic asteroid belt. Let’s dive in and watch the light wobble together!