Hostname: page-component-cd9895bd7-lnqnp Total loading time: 0 Render date: 2024-12-19T02:46:43.386Z Has data issue: false hasContentIssue false
  • English
  • Français

Radial Pulsation in Variable Stars with Mass Loss

Published online by Cambridge University Press:  12 April 2016

Frank P. Pijpers
Frank P. Pijpers*
Affiliation:
Astronomy Unit, School of Mathematical Sciences, Queen Mary and Westfield College, Mile End Road, London El 4NS, UK

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

It is possible to show that cool giants with very large photospheric scale heights do not perfectly reflect pulsational waves at the photosphere. This means that for these stars the classical formulation of pulsation in which the outer boundary for the resonance cavity is assumed to be perfectly reflecting is not valid. This can have significant consequences for the eigenfrequencies of the pulsation of Long Period Variables such as Mira type variables as well as for the stability of their pulsation.

Type
VI. Asteroseismology: theory
Information
International Astronomical Union Colloquium , Volume 137: Inside the Stars , 1993 , pp. 575 - 577
Copyright
Copyright © Astronomical Society of the Pacific 1993

References

Keeley, D.A., 1970, Ap. J.,, 161, 643 Google Scholar
Pijpers, F.P., 1992, in preparationGoogle Scholar
Pijpers, F.P., Habing, H.J., 1989, Astr. Ap.,, 215, 334 Google Scholar
Wood, P.R., 1974, Ap. J.,, 190, 609 CrossRefGoogle Scholar
Wood, P.R., 1990, In Proceedings of the International Colloqium From Miras to Planetary Nebulae: which path for stellar evolution ?, ed. Mennessier, O. and Omont, A., Editions Frontieres, Gif sur Yvette, p. 67 Google Scholar