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Planets have been detected orbiting several solar-type stars using high-precision radial velocity (v r) measurements. While changes in v r can be measured with an accuracy of a few m s \1, there has been relatively little study of how other astrophysical processes, such as magnetic activity, may effect the observed velocities. In this paper, we use published data and simple models to explore the contributions to v r from two activity-related sources, starspots and convective inhomogeneities, as these features rotate across the disk and evolve in time. Radial velocity perturbations due to both of these sources increase with rotation and the level of surface activity. Our models indicate that for solar-age G stars, the amplitude of perturbations due to spots is A S ¸ ! 5 m s \1, increasing to A S ¸ 30 to 50 m s \1 for Hyades-age G stars. If f S is the starspot area coverage, we find A S / f 0: 9 S v sin i. The effects of convective inhomogeneities (as observed. . .
Saar et al. (Sun,) studied this question.