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Non-radial Pulsation Modeling of ω (28) CMa

Published online by Cambridge University Press:  12 April 2016

M. Maintz ,
Th. Rivinius ,
S. Tubbesing ,
B. Wolf ,
S. Štefl  and
D. Baade
M. Maintz
Affiliation:
Landessternwarte Königstuhl, Heidelberg, Germany
Th. Rivinius
Affiliation:
Landessternwarte Königstuhl, Heidelberg, Germany
S. Tubbesing
Affiliation:
Landessternwarte Königstuhl, Heidelberg, Germany
B. Wolf
Affiliation:
Landessternwarte Königstuhl, Heidelberg, Germany
S. Štefl
Affiliation:
Astronomical Institute, Academy of Sciences of the Czech Republic
D. Baade
Affiliation:
European Southern Observatory, Garching, Germany

Abstract

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Adopting non-radial pulsation (nrp) the line profile variability lpv of several absorption lines of different ions was modeled for ω (28) CMa. The parameters suggested by Baade (1982) to characterise the pulsation could be confirmed. The pulsation period in the inertial frame was found to be negative, i.e. an actually retrograde mode appears prograde due to the rapid stellar rotation. The line profiles could be reproduced in detail including structures like spikes and ramps. They were identified as velocity effect due to the latitudinal component of the nrp velocity field υϑ in combination with low inclination i. In spite of small photometric variations (Štefl et al. 1999) the lpv of the absorption lines can be explained by nrp entirely.

Type
3. Periodic Variations
Information
International Astronomical Union Colloquium , Volume 175: The Be Phenomenon in Early-Type Stars , 2000 , pp. 244 - 247
Copyright
Copyright © Astronomical Society of the Pacific 2000

References

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