A Search for Line Shape and Depth Variations in 51 Pegasi and Tau Bootis

Abstract

Spectroscopic observations of 51 Pegasi and tau Bootis show no periodic changes in the shapes of their line profiles; these results for 51 Peg are in significant conflict with those reported by Gray and Hatzes (1997). Our detection limits are small enough to rule out nonradial pulsations as the cause of the variability in tau Boo, but not in 51 Peg. The absence of line shape changes is consistent with these stars' radial velocity variability arising from planetary-mass companions.

arXiv comment10 pages, 2 figures, plain TeX, accepted for publication in ApJL

References in corpus (1)

• A Planet Orbiting the Star Rho Coronae Borealis

Cited by in corpus (5)

• Extra-Solar Planets
• Searching for Planets in the Hyades II: Some Implications of Stellar Magnetic Activity
• Exoplanets or Dynamic Atmospheres? The Radial Velocity and Line Shape Variations of 51 Pegasi and Tau Bootis
• Spectral Line Distortions in the Presence of a Close-In Planet
• A Search for Variability in the Spectral Line Shapes of tau Bootis: Does this Star Really Have a Planet?