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Fig. 6.

image

Sketch of the Be outburst of HD 49330. In the quiescent phase, p modes are present and g modes stochastically excited at the interface between the convective core and the radiative envelope transport momentum towards the surface. Once enough momentum has accumulated, transient g modes get excited in the surface layer while p modes are destabilised and thus disappear. An ejection of material finally occurs. The star then relaxes back to a quiescent phase and p modes reappear.

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