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Energy of solar-like oscillations in red giants

Published online by Cambridge University Press:  18 February 2014

Mathieu Grosjean ,
Marc-Antoine Dupret ,
Kevin Belkacem ,
Josefina Montalbán  and
Reza Samadi
Mathieu Grosjean
Affiliation:
Institut d'astrophysique et de géophysique, Université de Liège, Allée du 6 Août 17, B-4000 Liège, Belgium email: grosjean@astro.ulg.ac.be
Marc-Antoine Dupret
Affiliation:
Institut d'astrophysique et de géophysique, Université de Liège, Allée du 6 Août 17, B-4000 Liège, Belgium email: grosjean@astro.ulg.ac.be
Kevin Belkacem
Affiliation:
LESIA Observatoire de Paris-Meudon, 5 place Jules Janssen, F-92195 Meudon, France
Josefina Montalbán
Affiliation:
Institut d'astrophysique et de géophysique, Université de Liège, Allée du 6 Août 17, B-4000 Liège, Belgium email: grosjean@astro.ulg.ac.be
Reza Samadi
Affiliation:
LESIA Observatoire de Paris-Meudon, 5 place Jules Janssen, F-92195 Meudon, France
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Abstract

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CoRoT and Kepler observations of red giants reveal a large variety of spectra of nonradial solar-like oscillations. So far, we understood pretty well the link between the global properties of the star (radius, mass, evolutionary state) and the properties of the oscillation spectrum (Δν, νmax, period spacing). We are interested here in the theoretical predictions of two other components of a power spectrum, the mode linewidths and heights. The study of the energy of the oscillations is of great importance to predict the peak parameters in the power spectrum. We will discuss circumstances under which mixed modes are detectable for red-giant stellar models from 1 to 2 M⊙, with emphasis on the effect of the evolutionary status of the star along the red-giant branch on theoretical power spectra.

Keywords

red giantssolar-like oscillationsmixed-mode lifetimes
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Symposium S301: Precision Asteroseismology , August 2013 , pp. 341 - 344
Copyright
Copyright © International Astronomical Union 2014 

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