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Title:
Stellar and circumstellar activity of the Be star omega CMa. III. Multiline non-radial pulsation modeling
Authors:
Maintz, M.; Rivinius, Th.; Štefl, S.; Baade, D.; Wolf, B.; Townsend, R. H. D.
Affiliation:
AA(Landessternwarte Königstuhl, 69117 Heidelberg, Germany), AB(Landessternwarte Königstuhl, 69117 Heidelberg, Germany; European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching bei München, Germany), AC(Astronomical Institute, Academy of Sciences, 251 65 Ondřejov, Czech Republic), AD(European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching bei München, Germany), AE(Landessternwarte Königstuhl, 69117 Heidelberg, Germany), AF(Department of Physics & Astronomy, University College London, Gower Street, London WC1E 6BT, UK)
Publication:
Astronomy and Astrophysics, v.411, p.181-191 (2003) (A&A Homepage)
Publication Date:
11/2003
Origin:
A&A
A&A Keywords:
stars: oscillations, stars: individual: omega (28) CMa
DOI:
10.1051/0004-6361:20031375
Bibliographic Code:
2003A&A...411..181M

Abstract

The line profile variability of omega CMa is modeled for various photospheric absorption lines of different ions as non-radial pulsation. The retrograde pulsation suggested by \citet{1982A&A...105...65B} could be confirmed. Due to rapid rotation, the line profile variability appears prograde, however. The line profiles could be reproduced in great detail, including prominent structures like ``spikes'' and ``ramps''. These features arise naturally from the pole-on orientation of the star together with high-amplitude pulsation in g-modes, i.e. with horizontal motions being dominant. The change of the line profile variability during outbursts (understood as the beginning of phases of high brightness) reported in \citetalias{paper2} of this series can also be understood within the framework of non-radial pulsation if veiling effects of the circumstellar disk are taken into account. It is concluded that the coherent periodic line profile variability of the absorption lines of omega CMa can be explained by non-radial pulsation in detail.

Based on observations collected at the European Southern Observatory at La Silla, Chile, 55.D-0502, 56.D-0381, 58.D-0697, 62.H-0319, 64.H-0548, and 267.D-5702.

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