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Radial Velocity Variability of K Giants

Published online by Cambridge University Press:  12 April 2016

Artie P. Hatzes  and
William D. Cochran
Artie P. Hatzes
Affiliation:
McDonald Observatory, The University of Texas, Austin Texas 78712, USA
William D. Cochran
Affiliation:
McDonald Observatory, The University of Texas, Austin Texas 78712, USA

Abstract

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At McDonald Observatory we have been monitoring the relative radial velocities of a sample of K giants. The technique employed uses the telluric O2 lines near 6300 Å as a reference for measuring the stellar line shifts. We demonstrate that precisions of 10 m s−1 are possible with this technique. We present radial velocity data covering a 2 year time span for α Boo, α Tau, and β Gem. All of these stars show both long term variations (~ several hundred days) with a peak-to-peak amplitude of about 400 m s−1 and short term variations (~ few days) with a peak-to-peak amplitude of about 100 m s−1. The long term variations may be due to the rotational modulation of surface active regions whereas the short term variations may be indicative of pulsations.

Type
Part IV Stellar activity
Information
International Astronomical Union Colloquium , Volume 130: The Sun and Cool Stars: activity, magnetism, dynamos , 1991 , pp. 386 - 388
Copyright
Copyright © Springer-Verlag 1991

References

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