Volume 543, July 2012
|Number of page(s)||8|
|Section||Stellar structure and evolution|
|Published online||09 July 2012|
Amplitudes of solar-like oscillations in red giant stars
Evidence for non-adiabatic effects using CoRoT observations
1 LESIA, CNRS UMR 8109, Observatoire de Paris, Université Pierre et Marie Curie, Université Denis Diderot, Place Jules Janssen, 92195 Meudon Cedex, France
2 Institut d’Astrophysique et de Géophysique de l’Université de Liège, Allée du 6 Août 17, 4000 Liège, Belgium
3 Zentrum für Astronomie der Universität Heidelberg, Landessternwarte, Königstuhl 12, 69117 Heidelberg, Germany
4 GEPI, CNRS, Observatoire de Paris, Université Denis Diderot, Place Jules Janssen, 92195 Meudon Cedex, France
5 Institut d’Astrophysique Spatiale, CNRS, Université Paris XI, 91405 Orsay Cedex, France
Received: 21 March 2012
Accepted: 18 May 2012
Context. A growing number of solar-like oscillations has been detected in red giant stars thanks to the CoRoT and Kepler space-crafts. In the same way as for main-sequence stars, mode driving is attributed to turbulent convection in the uppermost convective layers of those stars.
Aims. The seismic data gathered by CoRoT on red giant stars allow us to test the mode driving theory in physical conditions different from main-sequence stars.
Methods. Using a set of 3D hydrodynamical models representative of the upper layers of sub- and red giant stars, we computed the acoustic mode energy supply rate (). Assuming adiabatic pulsations and using global stellar models that assume that the surface stratification comes from the 3D hydrodynamical models, we computed the mode amplitude in terms of surface velocity. This was converted into intensity fluctuations using either a simplified adiabatic scaling relation or a non-adiabatic one.
Results. From L and M (the luminosity and mass), the energy supply rate is found to scale as (L/M)2.6 for both main-sequence and red giant stars, extending previous results. The theoretical amplitudes in velocity under-estimate the Doppler velocity measurements obtained so far from the ground for red giant stars by about 30%. In terms of intensity, the theoretical scaling law based on the adiabatic intensity-velocity scaling relation results in an under-estimation by a factor of about 2.5 with respect to the CoRoT seismic measurements. On the other hand, using the non-adiabatic intensity-velocity relation significantly reduces the discrepancy with the CoRoT data. The theoretical amplitudes remain 40% below, however, the CoRoT measurements.
Conclusions. Our results show that scaling relations of mode amplitudes cannot be simply extended from main-sequence to red giant stars in terms of intensity on the basis of adiabatic relations because non-adiabatic effects for red giant stars are important and cannot be neglected. We discuss possible reasons for the remaining differences.
Key words: stars: solar-type / stars: oscillations / sun: oscillations / turbulence / convection / waves
© ESO, 2012
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