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Spectroscopic monitoring of RS CVN stars at Kitt Peak using the Penn State Fiber Optic Echelle

  • Lawrence W. Ramsey
  • David P. Huenemoerder
  • Derek L. Buzasi
  • Samuel C. Barden
Contributed Papers on Active Binary Stars
Part of the Lecture Notes in Physics book series (LNP, volume 291)

Abstract

The Penn State Fiber Optic Echelle has been moved to Kitt Peak and works with either the coude feed telescope or 2.1 meter. It is about twice as efficient as the coude Camera No. 5 for similar bandpass at 600 nm and is comparable at 400 nm using the coude feed telescope. The high illumination stability afforded by the fiber is a decided advantage where spectrophotometric and radial velocity stability are at a premium, as in the study of active stars. We are using this instrument to intensively monitor about 10 regular RS CVn systems and about six short period and W UMa systems for a two week period each observing semester.

Keywords

Active Star Balmer Line Echelle Spectrograph Phase Coverage Hydrogen Balmer Line 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

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References

  1. Hall, D.S. 1980, in “Solar Phenomena in Stars and Stellar Systems”, ed. R.M. Bonnet and A.K. Dupree (Dordrecht: Reidel), p. 431.Google Scholar
  2. Huenemoerder, D.P. 1987, this volume.Google Scholar
  3. Huenemoerder, D.P. and Ramsey, L.W. 1987, Ap. J. 319, 392.Google Scholar
  4. Linsky, J.L. 1984, in “Cool Stars, Stellar Systems and the Sun”, ed. S. Baliunas and L. Hartmann (Berlin: Springer-Verlag), p. 244.Google Scholar
  5. Ramsey, L.W. and Huenemoerder, D.P. 1986, S.P.I.E. 627, p. 282.Google Scholar

Copyright information

© Springer-Verlag 1987

Authors and Affiliations

  • Lawrence W. Ramsey
    • 1
  • David P. Huenemoerder
    • 1
  • Derek L. Buzasi
    • 1
  • Samuel C. Barden
    • 2
  1. 1.Pennsylvania State UniversityUSA
  2. 2.Kitt Peak National ObservatoryUSA

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