Non-radial modes in AGB stars
1 Department of Physics and Astronomy “Galileo Galilei”, University of Padua, Vicolo dell’Osservatorio 3, I-35122 Padova, Italy
2 Research School of Astronomy and Astrophysics, Australian National University, Canberra, ACT2611, Australia
3 Observatory of Padua-INAF, Vicolo dell’Osservatorio 5, I-35122 Padova, Italy
Published online: 8 September 2017
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.
© The Authors, published by EDP Sciences, 2017