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Problems with the Pulsation Mode Selection Mechanism in the Lower Instability Strip (Observations and Theory)

Published online by Cambridge University Press:  12 April 2016

M. Breger  and
A.A. Pamyatnykh
M. Breger
Affiliation:
Institut für Astronomie, Universität Wien, Türkenschanzstr. 17, A-1180 Wien, Austria; email:breger@astro.univie.ac.at
A.A. Pamyatnykh
Affiliation:
Institut für Astronomie, Universität Wien, Türkenschanzstr. 17, A-1180 Wien, Austria; email:breger@astro.univie.ac.at Copernicus Astronomical Center, Bartycka 18, 00-716 Warsaw, Poland; email:alosza@camk.edu.pl Institute of Astronomy, Russian Academy of Sciences, Pyatnitskaya 48, 109017 Moscow, Russia

Abstract

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We examine the severe disagreement between the number of predicted and observed pulsation modes for δ Scuti stars. The selection of nonradial modes trapped in the outer envelope is considered on the basis of kinetic energy arguments. The trapped l = 1 modes for the star 4 CVn are in good, but not perfect agreement with the observations. The trapping of the l = 2 modes is weaker, so that this simple rule of mode selection may apply to l = 1, and possibly not to l = 2 modes.

Type
Part 3. Nonlinear Effects in Pulsating Stars
Information
International Astronomical Union Colloquium , Volume 185: Radial and Nonradial Pulsations as Probes of Stellar Physics , 2002 , pp. 388 - 391
Copyright
Copyright © Astronomical Society of the Pacific 2002

References

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