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Long-Termed Variability in the Far Ultraviolet Flux of Be Stars

Published online by Cambridge University Press:  23 September 2016

G. J. Peters  and
R. S. Polidan
G. J. Peters
Affiliation:
Space Sciences Center, University of Southern California, Los Angeles, CA 90089-1341; USA
R. S. Polidan
Affiliation:
Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721; USA

Extract

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Optical light variability appears to be commonplace in Be stars, on time scales from days to decades, but the phenomenon has yet to be satisfactorily explained. Some possible causes include changes in 1) the star's photospheric temperature or radius, or 2) the envelope's opacity or continuous emission. To investigate the nature of the photometric variability in Be stars, we have been monitoring the FUV flux of selected objects with the ultraviolet spectrometers (UVS) on the Voyager 1 and 2 spacecrafts (cf. Broadfoot, et al. 1977, and Holberg, et al. 1982, respectively, for information on the instrumentation and calibration, and Drilling, et al. 1984 and Polidan, et al. 1987 for a discussion of data reduction techniques), and report the initial results from these observations in this paper.

Type
III. The Circumstellar Gas
Information
International Astronomical Union Colloquium , Volume 92: Physics of Be Stars , August 1987 , pp. 278 - 281
Copyright
Copyright © Cambridge University Press 1987

References

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