Fig. 6.

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Method used to assess the power injected into stellar acoustic modes. We first computed a stellar model with MESA, where the modification of the stellar structure by rotation is not taken into account. For a given value of rotation Ω, we compute the local Rossby number and then the modified convective wavenumber and velocity, following the prescriptions by Augustson & Mathis (2019). We compute the eigenfunctions and eigenfrequencies for the acoustic modes using GYRE. It enables us to compute at each radius position the local spectral source term . Finally, we integrate the resulting contribution on the whole Convective Zone (CZ).
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