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Non-radial Pulsation Modeling of μ Centauri

Published online by Cambridge University Press:  12 April 2016

Th. Rivinius
Th. Rivinius*
Affiliation:
Landessternwarte Königstuhl, D-69117 Heidelberg, Germany

Abstract

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It is shown that the line profile variability (lpv) of μ Cen can be modeled as non-radial pulsations (nrp). The use of the most recent available modeling technique for the nrp and carefully computed stellar observables (intrinsic line profile and flux) are, however, mandatory to take full advantage of present high-quality data.

Type
3. Periodic Variations
Information
International Astronomical Union Colloquium , Volume 175: The Be Phenomenon in Early-Type Stars , 2000 , pp. 228 - 231
Copyright
Copyright © Astronomical Society of the Pacific 2000

References

Balona, L.A., Aerts, C., Štefl, S. 1999, MNRAS 305, 519 CrossRefGoogle Scholar
Baschek, B., Holweger, H., Traving, G. 1966, Abh. d. Hamb. Sternw. 8-1, 26 Google Scholar
Cuypers, J, Balona, L.A., Marang, F. 1989, A&AS 81, 151 Google Scholar
Diaz-Cordovés, J., Claret, A., Giménez, A. 1995, A&AS 110, 329 Google Scholar
Gummersbach, C.A., Kaufer, A., Schäfer, D.R., et al. 1998, A&A 338, 881 Google Scholar
Rivinius, Th., Baade, D., Štefl, S., et al. 1998, A&A 336, 177 Google Scholar
Townsend, R.H.D. 1997, MNRAS 284, 839 CrossRefGoogle Scholar