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The Saha Equation

Our calculations yesterday assumed that all the hydrogen atoms in a star's photosphere were neutral; or, more accurately, it provided the ratio of neutral atoms in the n=2 state to the n=1 state. But what if the number of neutral atoms changes drastically from A stars to B stars? That might cause there to be many more neutral atoms in the n=2 state in an A star, even if its temperature is lower than that of a B star.