ABSTRACT
The line-profile variations of the rapidly rotating delta Scuti star gamma Boo can be explained by high-degree (|m| /= 10) nonradial pulsations (NRPs) with an apparent period of Delta t /= 0.047 days. This same period was derived from two data sets taken three months apart where-in the amplitude increased by 30%. Such high-degree NRP cannot explain the apparent reversals previously observed (Auvergne, Le Contel & Baglin 1979) for this star in the cores of the hydrogen Balmer lines and CaII K line. Our radial-velocity variations can be reconciled with their 0.25 day spectroscopic period if an amplitude of 1 km s-1 is adopted, an order of magnitude less than previous measurements. We demonstrate that the presence of line-profile variations from high-degree modes probably limits the accuracy of radial-velocity measurements and may appear as bumps in the radial-velocity curve.