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Fig. 4.


Top: independent pulsation periods of the star plotted versus radial overtone number k. The least-squares line fit to k >  5 (using the mean period of f3 and f5 for k = 13; black) indicates a roughly constant period spacing consistent with dipole ℓ = 1 modes. The transparent gray lines represent fits to the perturbed periods assuming different observed azimuthal orders, m (see text). Middle: residuals of the linear fit shows evidence of a possible mode trapping cycle. We label the mode IDs from Table 1. Bottom: pulsation spectrum in period space with the dotted vertical lines indicating the expected locations of ℓ = 1 modes from the asymptotic pulsation theory given our least-squares fit parameters.

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