An emission feature at 1026‐Å observed at 600 km in the dayglow with a spectrometer on board the STP 78‐1 spacecraft cannot be explained by geocoronal hydrogen Lyman β. An accidental resonance of some lines of the O I multiplet at 1026‐Å with the broad solar Lyman β line can in fact account for the observed emission rate, based on analysis with a Monte Carlo radiative transport model. Photoelectron excitation of atomic oxygen is negligible compared with resonant scattering. These airglow results support a ratio of 66 to 1 for the solar Lyman α to Lyman β line center fluxes.
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Meier et al. (1987) studied this question.
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