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Title: Stellar pulsation and the RV Tauri phenomenon
Author: Worrell, John Kingsley
ISNI:       0000 0004 2738 1456
Awarding Body: University of St Andrews
Current Institution: University of St Andrews
Date of Award: 1985
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On the basis of observational data it is argued that RV Tauri variables, and probably yellow semiregular (SRd) variables, are closely related in every way to type II cepheid stars. Assuming that a single mass (~O.6 M~) is applicable to all three classes of star linear, nonadiabatic pulsation models are calculated. Using these models, the observed effective temperatures, and periods for these stars new luminosities are calculated and compared with the observed luminosities. This comparison appears to confirm the relationships between the three classes implied by the observations for the globular cluster stars. It is shown that an interaction of two or more pulsation modes could be responsible for the characteristic light curves of the RV and SRd stars but it is argued that this is unlikely. One RV star and a high luminosity F star both exhibit pulsations with two periods. The periods together with the observed effective temperatures and linear pulsation calculations yield masses and luminosities for the two stars. On the basis of the linear pulsation calculations the peculiar characteristics of the pulsations are explained. A sequence of nonlinear pulsation models based on the "standard" physics is presented. The light curves for some of these models show features characteristic of the RV stars. Strange behaviour found in the luminosity at the surface of some models is shown to be a product of an inadequate boundary condition. An alternative is suggested which cures the problem. Nonlinear models calculated with the new boundary condition eject matter, form very extended atmospheres, exhibit semiregular RV - like light curves with a (possibly) cyclic variation of the phase of light minima, and show long term variations of mean effective temperature. strong shock waves exhibiting properties like those found in RV stars are found. It is suggested that the equilibrium diffusion approximation is inappropriate for these models and the consequences of its use discussed.
Supervisor: Carson, T. R. Sponsor: Not available
Qualification Name: Thesis (Ph.D.) Qualification Level: Doctoral
EThOS ID:  DOI: Not available
Keywords: QB838.T2W7