  So far, solar-like oscillations have been studied using radial velocity
and/or light curve variations, which reveal frequencies of the oscillation
modes. Line-profile variations, however, are also a valuable diagnostic to
characterise radial and non-radial oscillations, including frequencies,
amplitudes, the spherical mode wavenumbers (l,m) and the stellar inclination
angle. Here we present a line profile analysis of epsilon Ophiuchi, which is a
pulsating red giant. The main differences compared to previous line profile
analyses done for heat-driven oscillations are the small amplitudes and the
predicted short damping and re-excitation times in red giants.
  Two line diagnostics have been tested to see whether these are sensitive to
the small line profile variations present in red giants. In addition, line
profiles have been simulated with short damping and re-excitation times and are
compared with the observations. This comparison reveals that non-radial modes
are detected in the observed line profile variations of epsilon Ophiuchi. This
is rather surprising, as theoretical predictions favours the occurrence of
radial modes.
