LONG-PERIOD RADIAL-VELOCITY VARIATIONS IN 3 K-GIANTS

Precise relative radial velocities (sigma approximately 20 m s-1) are presented for three K giants: alpha Tau, alpha Boo, and beta Gem. The data reveal periods of 233 days for alpha Boo, 643 days for alpha Tau, and 558 days for beta Gem. These periods are much too long to be due to radial pulsations. Currently, the only plausible explanations for t hese radial velocity variations are that they are due to rotational mo dulation by surface features (the expected rotation periods for these stars are of order the observed periods), nonradial pulsations, or pla netary companions. Orbital solutions to the radial velocity variations yield companion masses in the range of 3 to 12 Jovian masses. However , the fact that all three stars exhibit similar periods and give compa rable companion masses suggests that the variability is intrinsic to t he star (either rotational modulation or pulsations). Phasing the radi al velocity measurements of a Boo and a Tau by Walker et al. to our ep hemeris results in a good agreement in both phase and amplitude with o ur radial velocity data. These long-term variations seem to have been present and coherent for at least the last 10 yr. The period of the re lative radial velocity variations for a Boo is identical to the period of He I 10830 angstrom variations found by Lambert. This indicates th at the observed radial velocity variations may be related to the chrom ospheric heating in these stars. Alpha Boo and alpha Tau show signific ant night-to-night changes in the radial velocity of up to 100 m s-1. This indicates the presence of short-term periods. However, the sampli ng pathology of our data is such that these periods cannot be well det ermined. Beta Gem shows no significant night-to-night variations.