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Astero-Oscillometry: Gauging Stars with Oscillations1

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

Abstract

Astero-oscillometry is presented as a new method for deriving stellar parameters on the basis of a physical modeling of line profile variability (lpv) caused by nonradial pulsation (nrp). First applications to rapidly rotating B-type stars show that the method is able to yield reasonable stellar parameters. The radii are systematically smaller compared to those derived by conventional methods. This could be attributed to possible effects of rapid rotation on stellar evolution. Since the method requires only one or a few pulsation modes to be excited, it is ideally suited to investigating early-type stars.

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Copyright

Footnotes

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1

Based on observations obtained at the European Southern Observatory, La Silla, Chile, prop. Nos. 62.H-0319 and 64.H-05481

Footnotes

References

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Claret, A. 1995, A&AS, 109, 441
Gummersbach, C.A., Kaufer, A., Schäfer, D.R., Szeifert, T., & Wolf, B. 1998, A&A, 338, 881
Maintz, M., Rivinius, Th., Tubbesing, S., & Wolf, B. 2000, in ASP Conf. Ser., Vol. 214, The Be Phenomenon in Early-Type Stars, eds. Smith, H., Henrichs, M., & Fabregat, J., 244
Rivinius, Th., Baade, D., Steri, S., Townsend, R.H.D., Stahl, O., Wolf, B., & Kaufer, A., 2001, A&A, 369, 1058
Townsend, R.H.D. 1997, MNRAS, 284, 839

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