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Fig. 10


Radial velocity curves from the metallic lines of TU UMa from different publications phased with the pulsation period corrected for the LiTE and secular period changes. Uncorrected observed RVs (top) and corrected values after subtracting the changes in RV caused by orbital motion based on our model 1 (bottom). RV values corrected for binary orbit are evidently less scattered than uncorrected RVs.

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