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Short period line profile and light variations in the Be star ω Orionis

Balona, L.A. ; Aerts, C. ; Božić, H. ; Guinan, E.F. ; Handler, G. ; James, D.J. ; Kaye, A.B. ; Shobbrook, R.R.

In: Monthly Notices of the Royal Astronomical Society, 2001, vol. 327, no. 4, p. 1288-1296

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    Titre
    • Short period line profile and light variations in the Be star ω Orionis
    Auteur
    • Balona, L.A.. South African Astronomical Observatory, PO Box 9, Observatory 7935, Cape Town, South Africa
    • Aerts, C.. Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Leuven, Belgium
    • Božić, H.. Hvar Observatory, Faculty of Geodesy, Zagreb University, Kačićeva 26, 10000 Zagreb, Croatia
    • Guinan, E.F.. Astronomy and Astrophysics Department, Villanova University, Villanova, PA 19085, USA
    • Handler, G.. South African Astronomical Observatory, PO Box 9, Observatory 7935, Cape Town, South Africa
    • James, D.J.. School of Physics and Astronomy, University of St. Andrews, North Haugh, St. Andrews, Fife KY16 9SS
    • Kaye, A.B.. Applied Physics Division, X-5, Los Alamos National Laboratory, USA
    • Shobbrook, R.R.. Research School of Astronomy and Astrophysics, Australian National University, Canberra, ACT, Australia
    Type de document
    • Postprint
    Langue
    • Anglais
    Publié dans
    • Monthly Notices of the Royal Astronomical Society, 2001, vol. 327, no. 4, p. 1288-1296. Blackwell Science Ltd
    Autre version électronique
    Identifiant OAI-PMH
    • oai:doc.rero.ch:302714
    Summary
    We present the results of a multisite spectroscopic and photometric campaign on the Be star ω Orionis. From the photometry and radial velocity variation of several spectral lines, we confirm that the star is a variable with period . Only one period can be extracted from both the photometric and radial velocity observations. We find that the projected rotational velocity from the helium lines is considerably smaller than from the metal lines . The line profiles show an excess absorption feature moving from blue to red for half the period and from red to blue for the other half of the period. Another excess absorption feature moves exactly out of phase. The excess absorption features are present in photospheric lines as well as in lines which are significantly affected by circumstellar material, such as Hβ. From this we conclude that the periodic variations are most probably associated with corotating circumstellar material