51 Pegasi and Tau Boötis: Planets or Pulsations?

Scott D. Horner
Pennsylvania State University
Timothy M. Brown, Edward Kennelly, & R. Kotak
High Altitude Observatory
Saurabh Jha, Sylvain G. Korzennik, Peter Nisenson, & Robert W. Noyes
Harvard-Smithsonian Center for Astrophysics

Abstract

It has recently been suggested (Gray 1997) that the radial velocity variations observed in the spectra of 51 Pegasi are the result of stellar pulsations as opposed to the reflex motion due to an orbital companion. The AFOE group has confirmed the radial velocity variations in 51 Pegasi and tau Bootis. Here we discuss the results of a search for evidence of pulsations in the AFOE data for these two stars, as well as attempt to clear up misconceptions regarding pulsations circulated as a result of the current debate about the nature of the 51 Pegasi radial velocity variations.

This poster with the figures was presented at The 10th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun , Cambridge, July 1997.
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Sylvain G. Korzennik (skorzennik@cfa.harvard.edu)

Last modified: Tue Aug 12 16:09:36 1997