Turbulent convection and pulsation stability of stars - II. Theoretical instability strip for Scuti and Doradus stars
arXiv:1808.09621 · doi:10.1093/mnras/stw047
Abstract
By using a non-local and time-dependent convection theory, we have calculated radial and low-degree non-radial oscillations for stellar evolutionary models with --3.0\,. The results of our study predict theoretical instability strips for Scuti and Doradus stars, which overlap with each other. The strip of Doradus is slightly redder in colour than that of Scuti. We have paid great attention to the excitation and stabilization mechanisms for these two types of oscillations, and we conclude that radiative mechanism plays a major role in the excitation of warm Scuti and Doradus stars, while the coupling between convection and oscillations is responsible for excitation and stabilization in cool stars. Generally speaking, turbulent pressure is an excitation of oscillations, especially in cool Scuti and Doradus stars and all cool Cepheid- and Mira-like stars. Turbulent thermal convection, on the other hand, is a damping mechanism against oscillations that actually plays the major role in giving rise to the red edge of the instability strip. Our study shows that oscillations of Scuti and Doradus stars are both due to the combination of mechanism and the coupling between convection and oscillations, and they belong to the same class of variables at the low-luminosity part of the Cepheid instability strip. Within the Scuti-- Doradus instability strip, most of the pulsating variables are very likely hybrids that are excited in both p and g modes.
16 pages, 20 figures, published 2016 February 19
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