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Fig. 16

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Top panel: continuum normalised flux maxima observed with φ in strong Hα (open symbols) and Hβ (dots) emission lines of MWC 314. The Hα maxima are divided by 24, and Hβ maxima by 6.75 for comparison. Bottom panel: blue/red emission peak ratio we observe in two permitted Fe ii emission lines formed in the circumbinary disc. The B/R variations of ±10% are due to orbital modulation of Doppler shifting line opacity, whereas the Hα and Hβ flux changes result from variability of the stellar continuum flux with φ.

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