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SIMULATIONS OF STELLAR RADIAL VELOCITY AND SPECTRAL LINE BISECTOR VARIATIONS: I. NONRADIAL PULSATIONS

The radial velocity and spectral variations are calculated for low-amplitude nonradial pulsations in slowly rotating stars (v sin i = 3 km s-1). Sectoral modes (l = -m) in the range l = 1-8 are considered. An empirical equation relating the pulsational amplitude to the "observed" stellar radial velocity amplitude is derived and this indicates that precise radial velocity techniques should be able to detect low-amplitude (<1 km s-1) pulsations for sectoral modes as high as l = 6. The spectral variations manifest themselves via changes in the span and curvature of the line bisector which are maximized for m = 4. These spectral variations can be used to distinguish between radial velocity variations due to pulsations from those due to the reflex motion of the star caused by the presence of a low-mass companion. However, these measurements require data taken at high resolution (lambda/delta-lambad > 100,000) and high signal-to-noise ratios (S/N > 500).