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Fig. 2.

image

Statistically significant observed frequencies of HD 49330 (bottom panel) during and outside of the outburst phase compared to the modelled frequencies in a nearly critically rotating B star (middle panel) of 10 M (left) and 13 M (right) calculated using rotational deformation based on Chandrasekhar-Milne’s expansion. Top panel: azimuthal order m of each frequency peak. The dashed line represents the approximate separation between p and g modes. Red full lines correspond to even modes and dashed blue lines to odd modes.

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