Stellar and circumstellar activity of the Be star omega CMa. III. Multiline non-radial pulsation modeling

Details Stellar and circumstellar activity of the Be star omega CMa. III. Multiline non-radial pulsation modeling Stellar and circumstellar activity of the Be star omega CMa. III. Multiline non-radial pulsation modeling

Nov 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003a%26a...411..181m&link_type=abstract

Astronomy and Astrophysics, v.411, p.181-191 (2003)

Astronomy and Astrophysics

Astrophysics

15

Stars: Oscillations, Stars: Individual: Omega (28) Cma

Scientific paper

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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