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Energetical aspects of solar-like oscillations in red giants

  • Asteroseismology
  • Red Giants
  • Physical
  • Chemical
  • Mathematical & Earth Sciences :: Space Science
  • Astronomy & Astrophysics [G05]
  • Physique
  • Chimie
  • Mathématiques & Sciences De La Terre :: Aérospatiale
  • Astronomie & Astrophysique [G05]
  • Earth Science
  • Physics


Precision Asteroseismology Celebration of the Scientific Opus of Wojtek Dziembowski Proceedings IAU Symposium No. 301, 2013 A.C. Editor, B.D. Editor & C.E. Editor, eds. c© 2013 International Astronomical Union DOI: 00.0000/X000000000000000X Energetical aspects of solar-like oscillations in red giants Mathieu Grosjean1†, Marc-Antoine Dupret1, Kevin Belkacem2, Josefina Montalban1, Reza Samadi2 1Institut d’astrophysique et de geophysique, Universite de Liege, Allee du 6 Aout 17, B-4000 Liege, Belgium email: [email protected] 2LESIA Observatoire de Paris-Meudon 5 place Jules Janssen, F-92195 Meudon, France Abstract. CoRoT and Kepler observations of red giants reveal a large variety of spectra of non-radial solar-like oscillations. So far, we understood the link between the global properties of the star and the properties of the oscillation spectrum (∆ν, νmax, period spacing). We are interested here in the theoretical predictions not only for the frequencies, but also for the other properties of the oscillations : linewidths and heights. The study of energetic aspects of these oscillations is of great importance to predict the mode parameters in the power spectrum. I will discuss under which circumstances mixed modes are detectable for red-giant stellar models from 1 to 2M�, with emphasis on the effect of the evolutionary status of the star along the red-giant branch on theoretical power spectra. Keywords. red giants, solar-like oscillations, mixed-modes lifetimes 1. Introduction In a first part we consider three stellar models of 1.5M� on the red giant branch (Fig1 ). These models have been investigated in the adiabatic case by Montalba´n et al. (2013) In a second part we selected models of 1, 1.7 and 2.1 M� which have the same number of mixed-modes in a large separation than the model B of 1.5M�(Fig1 ). All these models (see details in Table1) are computed with the code ATON ( Ventura et al. (2008)) using the MLT for the treatment of the convection with αMLT = 1.9. The

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