  Solar-like oscillations have been observed in numerous red giants from ground
and from space. An important question arises: could we expect to detect
non-radial modes probing the internal structure of these stars? We investigate
under what physical circumstances non-radial modes could be observable in red
giants; what would be their amplitudes, lifetimes and heights in the power
spectrum (PS)? Using a non-radial non-adiabatic pulsation code including a
non-local time-dependent treatment of convection, we compute the theoretical
lifetimes of radial and non-radial modes in several red giant models. Next,
using a stochastic excitation model, we compute the amplitudes of these modes
and their heights in the PS. Very distinct results are found depending on the
evolutionary status of the star.

Solar and Stellar Astrophysics