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\section{Mode Visibility}  Solar-like oscillations modes  are driven by stochastic energy input from turbulent near-surface convection. At its time-averaged equilibrium amplitude, the energy input and damping rates of the a  mode are equal \cite{Dupret_2009}. %Modes suppressed via the magnetic greenhouse effect have an extra source of damping determined Observed modes are created  by the rate at which energy leaks through the evanescent region separating the acoustic cavity from the g-mode cavity.   Waves standing waves  with angular frequency $\omega \sim \omega_{\rm max} = 2 \pi \nu_{\rm max}$ are excited via convective motions, the frequencies near $\nu_{\rm max}$. These  waves propagate downward as acoustic waves until their frequency is less than the local Lamb frequency for waves of angular degree $\ell$, i.e., until $\omega = L_l = \sqrt{l(l+1)} c_s/r$, where $c_s$ is the sound speed and $r$ is the radial coordinate. At this boundary, part of the wave flux is reflected, and part of it tunnels through.The wave resumes propagating inward as a gravity wave in the radiative core where $\omega < N$, with $N$ the Brunt-Vaisala frequency.  The wave resumes propagating inward as a gravity wave in the radiative core where $\omega < N$, with $N$ the Brunt-Vaisala frequency.  In normal red giants, wave energy that tunnels into the core eventually tunnels back out to produce the observed oscillation modes. We show here that the visibility of suppressed modes can be explained if wave energy leaking into the core never returns to the stellar envelope. The degree of wave transmission is determined by the tunneling integral through the evanescent region. The transmission coefficient is   \begin{equation}