Abstract
Walker et al. (1989) were the first to establish, using precise stellar radial velocity measurements, that K giant stars were a new class of variables. The variability of some of these stars can be quite complex showing several periods ranging from several hours to several hundreds of days. The long-period variations result from sub-stellar companions or rotational modulation, but the short-period variability certainly arises from stellar oscillations. We present recent of precise stellar radial velocity measurements (σ ≈ 6m s −1 ) of two oscillating K giant stars: β Oph and γ Dra. These stars show oscillation periods of hours (β Oph) and days (γ Dra). These periods are consistent with solar-like stellar oscillations, given the stellar properties of the star. Radial modes are a prime candidate for the type of oscillations in these stars.
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