Hα

LITHydrogen's Balmer-alpha line (n = 3 → 2) is at 656.28 nm in air; the NIST Handbook lists its fine-structure components at 6562.71–6562.85 Å. In emission nebulae, ionised hydrogen recombines and cascades through this line, which is why H II regions photograph deep red. Hβ (486.13 nm) adds a little blue-green; to the eye, many nebulae look greenish, from oxygen [O III], and only cameras show the red.

COMPUTEDBalmer wavelengths come from the Rydberg formula with R_H = 1.09678×10⁷ m⁻¹ (vacuum), converted to air with n ≈ 1.000277. The nebula colour is the CIE mix of Hα and Hβ at the slider ratio (MODEL; the real Balmer decrement in nebulae is about 2.86, Case B, cited from memory and unverified). Nesting: an orange ionising star, purple and green filaments, a yellow dust lane, a blue reflection fringe, the red H II shell, the void.

ioniseeye vs camera

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