Editing Openai/6897769e-4ee4-800f-aba5-69cca34f701c (section)

=== 1. Mie scattering / droplet size — compute full Mie angular intensity vs λ for a set of radius distributions and build the observed intensity I(λ,θ)I(\lambda,\theta)I(λ,θ). Then compute a visually relevant “center angle” (e.g., angle of peak intensity at each λ, then spectrum-weighted). This step is essential to move from geometric Dmin⁡(λ)D_{\min}(\lambda)Dmin(λ) to what an observer would see as the rainbow angle. I can do this next, but it requires either a small Mie solver (we can implement a basic one) or using a library (needs pip/install). ===
# Use high-precision refractive index tables (Hale & Querry, or refractiveindex.info datasets) across the full band and also include temperature dependence of n(λ,T)n(\lambda,T)n(λ,T). I used an analytic Sellmeier-style fit (good), but the more precise tables will tighten numbers.
# Use measured solar spectrum (with Fraunhofer lines) instead of a pure Planck function — that will give the exact real-Sun weighting and show if the Sun’s actual line structure moves the mean. I can fetch solar spectral data and rerun.
# Laboratory experiment design — measure the rainbow center with a controlled lamp (tunable color temperature) and a monodisperse droplet generator: that would be a clean experimental test.

If you’d like, I can take one of these next steps now (Mie modelling, precise n(λ)n(\lambda)n(λ) table, solar spectrum, or a small report for YT) — tell me which and I’ll do it.