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Pulsation Modes in Mira and Semiregular Variables

Published online by Cambridge University Press:  25 May 2016

Michael Feast
Michael Feast*
Affiliation:
Department of Astronomy, University of Cape Town, Rondebosch, 7700, South Africa

Abstract

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The most direct evidence for the pulsation mode of Mira and SR variables comes from the linear diameters derived from individual parallaxes and angular diameters, together with the observed periods. The data now available strongly suggest that most, if not all, Miras and SRs pulsate in the same mode. If comparison is made with conventional models, this mode is the first overtone. Uncertainties in deriving the pulsational radius of a Mira from the observations do not appear significant enough to affect this conclusion. Evidence from SRs and Miras in globular clusters supports this conclusion and shows that the pulsation mode does not depend on metallicity. Analysis of light curves leads to broadly the same conclusions, if less directly. The light curves indicate that periodicities other than the main one may also be present and that mode switching may occur in some stars.

Type
Part 2. Pulsation, Mass Loss, Cool Envelopes
Information
Symposium - International Astronomical Union , Volume 191: Asymptotic Giant Branch Stars , 1999 , pp. 108 - 116
Copyright
Copyright © Astronomical Society of the Pacific 1999 

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