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Non-radial Pulsation Modeling of ω (28) CMa

  • M. Maintz (a1), Th. Rivinius (a1), S. Tubbesing (a1), B. Wolf (a1), S. Štefl (a2) and D. Baade (a3)...

Abstract

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 υ ϑ 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.

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Copyright

References

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Baade, D. 1982, A&A 105, 65
Balona, L.A., Aerts, C., Štefl, S. 1999, MNRAS 305, 519
Gummersbach, C.A., Kaufer, A., Schäfer, D.R., et al. 1998, A&A 338, 881
Hermanec, P. 1998, A&A 334, 558
Kaufer, A., Stahl, O., Tubbesing, S., et al. 1999, The ESO Messenger 95, 8
Štefl, S., Aerts, C., Balona, L.A. 1999, MNRAS 305, 505
Townsend, R.H.D. 1997, MNRAS 284, 839

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