Relative power fractions of the radial, dipole, and quadrupole modes as a function of stellar mean density. The top row shows the relative power distribution across radial orders for each angular degree ℓ, calculated as $P_n^{\ell }/{\sum }_{{\ell }^{\mathrm{\prime }}}{P}_n^{{\ell }^{\mathrm{\prime }}}$. The black-lines in the leftmost panel indicate the fractions of the growth rates of the fundamental, first and second overtones relative to summed-up growth rates, providing a means of comparing the relative amplitudes derived from linear 1D models (Trabucchi et al. 2019), as described in Sect. 3.2. The bottom row displays the relative power for each angular degree at a given radial order n, calculated as $P_n^{\ell }/\sum n^{\mathrm{\prime }}{P}^{\ell }{n}^{\mathrm{\prime }}$. These plots illustrate how the dominant mode shifts depending on the mean density and radial order. Note that all power values are evaluated at the stellar surface for each identified mode.