Abstract
The success of asteroseismology in characterising G-K giants has motivated the extension of the same techniques to stars after the central He-burning and M-giants. The latter have been usually studied only as radial pulsators; the presence, however, of fine-structure in the period-luminosity diagram of red variables in the Magellanic Clouds could result from the presence of non-radial oscillations, offering the potential of observational indexes based on non-radial oscillations also for luminous red giants. We present here the results of a first approach aiming to identify the origin of the sub-ridges in the sequence A of the LMC red variables.
Highlights
After the central H- and He-burning, the density contrast between the core and the envelope increases with luminosity, and these stellar regions become dynamically decoupled
Radial and non-radial modes are strongly trapped in the envelope, and their oscillation frequencies are determined only by the physical properties of that region
We have verified its validity for dipole modes ( = 1) in 1.5 M AGB models, by computing = 1 frequency oscillations for complete and envelope models
Summary
After the central H- and He-burning, the density contrast between the core and the envelope increases with luminosity, and these stellar regions become dynamically decoupled. Radial and non-radial modes are strongly trapped in the envelope, and their oscillation frequencies are determined only by the physical properties of that region.
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