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

=== 1. Re-run the numerical experiment using a published, high-precision refractive-index table (Hale & Querry 1973 or Daimon & Masumura), plus a few realistic spectral shapes: - pure blackbody at several temperatures (Sunlike, cooler, hotter); - solar spectrum (observed solar continuum), - realistic plasma emission spectrum (observed line strengths; e.g., a hydrogen-dominated nebular spectrum), - measured ocean/atmosphere spectral transmission (if you want to model what actually reaches raindrops). ===
# Search for a short, clean geometric derivation (analytical) that estimates how a narrow line at λ0 changes the mean angle — gives an approximate formula for Δθ in terms of line amplitude and local slope dθ/dλ. (simple linear estimate: Δθ ≈ (fractional spectral weight at λ0) × dθ/dλ|λ0 — we can make that explicit and compare to the full integral.)
# If you like, I can produce a short, shareable write-up + plots (PNG/PDF) you can use in a YouTube/community post asking for independent checks (you asked about that earlier — I think it’s a fine idea). I can include the code and the precise references so other physicists can reproduce it quickly.