Hostname: page-component-cd9895bd7-hc48f Total loading time: 0 Render date: 2024-12-26T03:11:42.382Z Has data issue: false hasContentIssue false
  • English
  • Français

The Far Ultraviolet Spectra of υ Cyg and μ Cen

Published online by Cambridge University Press:  14 August 2015

Geraldine J. Peters
Geraldine J. Peters*
Affiliation:
Dept. of Astronomy, University of California, Los Angeles, Calif., U.S.A.
*
*Guest Investigator with the Princeton University telescope on the Copernicus satellite, which is sponsored and operated by the National Aeronautics and Space Administration.

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The spectra of the ‘pole-on’ Be stars υ Cyg and μ Cen have been observed in the region λλ 1000–1450 Å with the Princeton Ultraviolet Spectrometer on board the Copernicus satellite. The data include scans of intermediate resolution (0.2 Å) with U2 and high resolution scans (0.05 Å) of selected suspected shell lines with U1. The spectra of υ Cyg and μ Cen are compared with a complete intermediate resolution Copernicus scan of the equator-on Be star φ Per. The ultraviolet spectra of υ Cyg and μ Cen appear to be identical to those observed in non-Be stars of comparable ground-based spectral type. Neither emission nor shell features are observed. However, numerous strong shell features are seen in φ Per. An upper limit on the column density of hydrogen in our line of sight is computed for υ Cyg from the observed strength of a weak feature at λ 1130.4 Å identified as an Fe III shell line. Estimates for the dimensions of the circumstellar envelope are then obtained. Some implications of the strengths of the Fe III shell lines at λ 1130 Å observed in υ Cyg, μ Cen, φ Per, and other Be stars are discussed.

Type
Part III: New Observational Techniques
Information
Symposium - International Astronomical Union , Volume 70: Be and Shell Stars , 1976 , pp. 209 - 217
Copyright
Copyright © Reidel 1976 

References

Bohlin, R. C.: 1975, preprint.Google Scholar
Bowen, I. S.: 1947, Publ. Astron. Soc. Pacific 59, 196.CrossRefGoogle Scholar
Kurucz, R. L. and Peytremann, E.: 1975, Smithsonian Astrophysical Observatory Special Report No. 362. Google Scholar
Marlborough, J. M.: 1969, Astrophys. J. 156, 135.Google Scholar
Pagel, B. E. J.: 1960, Vistas in Astronomy 3, 203.Google Scholar
Peters, G. J.: 1976, this volume, p. 69.CrossRefGoogle Scholar
Rogerson, J. B., Spitzer, L., Drake, J. F., Dressler, K., Jenkins, E. B., Morton, D. C., and York, D. G.: 1973, Astrophys. J. Letters 181, L97.Google Scholar
Slettebak, A.: 1949, Astrophys. J. 110, 498.Google Scholar
Slettebak, A.: 1968, Astrophys. J. 151, 1043.Google Scholar
Slettebak, A. and Howard, R. F.: 1955, Astrophys. J. 121, 102.Google Scholar
Snow, T. P.: 1975, A Guide for Guest Investigators Using the Princeton Telescope on the Satellite COPERNICUS. Google Scholar
Uesugi, A. and Fukuda, I.: 1970, Contrib. Inst. Astrophys. Kwasan Obs. Univ. Kyoto , No. 189.Google Scholar