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The Magnetic Be Star Sigma Orionis E

Published online by Cambridge University Press:  23 September 2016

C. T. Bolton
Affiliation:
David Dunlap Observatory, Richmond Hill, Ontario L4C 4Y6
A. W. Fullerton
Affiliation:
David Dunlap Observatory, Richmond Hill, Ontario L4C 4Y6
D. Bohlender
Affiliation:
Department of Astronomy, University of Western Ontario London, Ontario N6A 5B9
J. D. Landstreet
Affiliation:
Department of Astronomy, University of Western Ontario London, Ontario N6A 5B9
D. R. Gies
Affiliation:
Astronomy Department, University of Texas, Austin, Texas 78712
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Extract

Over the past two years, we have obtained high resolution high signal/noise (S/N) spectra of the magnetic Be star σ Ori E at the Canada-France-Hawaii Telescope and McDonald Observatory. These spectra, which cover the spectral regions 399-417.5 and 440-458.5 nm and the Hα line and have typical S/N>200 and spectral resolution ≃0.02 nm, were obtained at a variety of rotational phases in order to study the magnetic field structure, the distribution of elements in the photosphere, and the effects of the magnetic field on the emission envelope. Our analysis of these spectra confirms, refines and extends the results obtained by Landstreet & Borra (1978), Groote & Hunger (1982 and references therein), and Nakajima (1985).

The Hα emission is usually double-peaked, but it undergoes remarkable variations with the 1.19081 d rotational period of the star, which show that the emitting gas is localized into two regions which co-rotate with the star.

Type
IIA. The Underlying Stars: Observations
Copyright
Copyright © Cambridge University Press 1987

References

Groote, D. & Hunger, K. (1982). Shell and Photosphere of σ Ori E: New Observations and Improved Model. Astr. Ap., 116, 6474.Google Scholar
Harmanec, P. (1986). In these proceedings.Google Scholar
Landstreet, J.D. & Borra, E.F. (1978). The Magnetic Field of Sigma Orionis E. Ap. J. Lett., 224, L5L8.CrossRefGoogle Scholar
Nakajima, R. (1985). The Circumstellar Gas of Sigma Orionis E. Ap. Space Sci., 116, 285297.Google Scholar

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