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Unified NRP-Modelling of Be Stars1

Published online by Cambridge University Press:  12 April 2016

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

Abstract

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Recently, the line profile variability (lpv) of two low-v sin i Be stars, μ Cen and ω (28) CMa was successfully modelled as nonradial pulsation (nrp) of rapidly rotating stars seen pole-on. In this work, it is shown that the lpv of low-v sin i early-type Be stars in general closely resembles these two cases, and is therefore explainable by the same mechanism. The lpv of intermediate to high-v sin i Be stars can be explained by the same model if the inclination angle of the model alone is increased. Consequently, early-type Be stars form a distinct, fairly homogeneous class of non-radial low-order g-mode pulsators.

Type
Part 2.2. B-Type Stars
Information
International Astronomical Union Colloquium , Volume 185: Radial and Nonradial Pulsations as Probes of Stellar Physics , 2002 , pp. 240 - 243
Copyright
Copyright © Astronomical Society of the Pacific 2002

Footnotes

1

Based on observations obtained at the European Southern Observatory, La Silla, Chile, prop. No. 64.H-0548, and Calar Alto observatory (DSAZ)

References

Maintz, M., Rivinius, Th., Tubbesing, S., Wolf, B., Štefl, S., & Baade, D. 2000, in ASP Conf. Ser., Vol. 214, The Be Phenomenon in Early-Type Stars, eds. Smith, M., Henrichs, H., & Fabregat, J., (San Francisco ASP), 244 Google Scholar
Rivinius, Th., Baade, D., Štefl, S., Townsend, R.H.D., Stahl, O., Wolf, B., & Kaufer, A. 2001, A&A, 369, 1058 Google Scholar
Townsend, R.H.D. 1997, MNRAS, 284, 839 Google Scholar