Abstract
CoRoT and Kepler observations of red giants reveal rich spectra of non-radial solar-like oscillations allowing to probe their internal structure. We compare the theoretical spectrum of two red giants in the same region of the HR diagram but in different evolutionary phases. We present here our first results on the inertia, lifetimes and amplitudes of the oscillations and discuss the differences between the two stars.
Highlights
We compare the theoretical spectrum of two red giants in the same region of the HR diagram but in different evolutionary phases
The two models considered in this study are a red giant branch (RGB) and a helium burning model (HB)
As already found by adiabatic computations [5], the spectrum density is larger in the RGB model
Summary
The two models considered in this study are a red giant branch (RGB) and a helium burning model (HB). CoRoT and Kepler observations of red giants reveal rich spectra of non-radial solar-like oscillations allowing to probe their internal structure. We compare the theoretical spectrum of two red giants in the same region of the HR diagram but in different evolutionary phases.
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