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IUE Spectra of RS CVn Stars

Published online by Cambridge University Press:  12 April 2016

A.D. Andrews
Affiliation:
Armagh Observatory, Armagh, N.Ireland
P.B. Byrne
Affiliation:
Armagh Observatory, Armagh, N.Ireland
C.J. Butler
Affiliation:
Armagh Observatory, Armagh, N.Ireland
J.L. Linsky
Affiliation:
JILA/NBS, University of Colorado, Boulder, USA
T. Simon
Affiliation:
JILA/NBS, University of Colorado, Boulder, USA
N. Marstad
Affiliation:
JILA/NBS, University of Colorado, Boulder, USA
M. Rodonò
Affiliation:
Osservatorio Astrofisico and Universita di Catania, Italy
C. Blanco
Affiliation:
Osservatorio Astrofisico and Universita di Catania, Italy
S. Catalano
Affiliation:
Osservatorio Astrofisico and Universita di Catania, Italy
E. Marilli
Affiliation:
Osservatorio Astrofisico and Universita di Catania, Italy
V. Pazzani
Affiliation:
Osservatorio Astrofisico and Universita di Catania, Italy

Extract

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The characteristic optical light curves of RS CVn - and BY Dra-type variables are believed to represent non-uniform distribution of dark spots akin to sunspots which are revealed by rotation. By analogy with the Sun, strong magnetic fields probably underlie this phenomenon, extending upwards into the chromosphere and corona, enhancing the emission from regions that overlie the spots. Previous work on the BY Dra variable AU Mic (Ref.l) did not clarify whether the fluxes from chromospheric and transition region lines were rotationally modulated in the sense that the phase of maximum emission was in register with spot visibility or minimum light. This important question prompted the need for further collaborative IUE, optical and radio work.

Type
Session III: Observed Activity in Related Objects
Copyright
Copyright © Reidel 1983

References

REFERENCES

1. Linsky, J.L. et al. 1982. Third European IUE Conference.Google Scholar
2. ESA Memorandum 1981. FES Calibration at Vilspa by Holm & Rice.Google Scholar