Volume 541, May 2012
|Number of page(s)||12|
|Section||Stellar structure and evolution|
|Published online||26 April 2012|
Evolutionary influences on the structure of red-giant acoustic oscillation spectra from 600d of Kepler observations
1 Instituut voor Sterrenkunde, K.U. Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium
2 Institute for Astronomy (IfA), University of Vienna, Türkenschanzstrasse 17, 1180 Vienna, Austria
3 Astronomical Institute “Anton Pannekoek”, University of Amsterdam, PO Box 94249, 1090 GE Amsterdam, The Netherlands
4 School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT, UK
5 LESIA, CNRS, Université Pierre et Marie Curie, Université Denis Diderot, Observatoire de Paris, 92195 Meudon Cedex, France
6 Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, NSW 2006, Australia
7 Department of Astronomy and Physics, Saint Marys University, Halifax, NS B3H 3C3, Canada
8 Department of Astronomy, Yale University, PO Box 208101, New Haven, CT 06520-8101, USA
9 Laboratoire AIM, CEA/DSM-CNRS, Université Paris 7 Diderot, IRFU/SAp, Centre de Saclay, 91191 Gif-sur-Yvette, France
10 SETI Institute/NASA Ames Research Center, Moffett Field, CA 94035, USA
11 Bay Area Environmental Research Inst./NASA Ames Research Center, Moffett Field, CA 94035, USA
Received: 20 January 2012
Accepted: 13 March 2012
Context. It was recently discovered that the period spacings of mixed pressure/gravity dipole modes in red giants permit a distinction between the otherwise unknown evolutionary stage of these stars. The Kepler space mission is reaching continuous observing times long enough to also start studying the fine structure of the observed pressure-mode spectra.
Aims. In this paper, we aim to study the signature of stellar evolution on the radial and pressure-dominated l = 2 modes in an ensemble of red giants that show solar-type oscillations.
Methods. We use established methods to automatically identify the mode degree of l = 0 and 2 modes and measure the large (Δνc) and small (δν02) frequency separation around the central radial mode. We then determine the phase shift ϵc of the central radial mode, i.e. the linear offset in the asymptotic fit to the acoustic modes. Furthermore we measure the individual frequencies of radial modes and investigate their average curvature.
Results. We find that ϵc is significantly different for red giants at a given Δνc but which burn only H in a shell (RGB) than those that have already ignited core He burning. Even though not directly probing the stellar core the pair of local seismic observables (Δνc, ϵc) can be used as an evolutionary stage discriminator that turned out to be as reliable as the period spacing of the mixed dipole modes. We find a tight correlation between ϵc and Δνc for RGB stars and unlike less evolved stars we find no indication that ϵc depends on other properties of the star. It appears that the difference in ϵc between the two populations becomes smaller and eventually indistinguishable if we use an average of several radial orders, instead of a local, i.e. only around the central radial mode, large separation to determine the phase shift. This indicates that the information on the evolutionary stage is encoded locally, more precisely in the shape of the radial mode sequence. This shape turns out to be approximately symmetric around the central radial mode for RGB stars but asymmetric for core He burning stars. We computed radial mode frequencies for a sequence of red-giant models and find them to qualitatively confirm our findings. We also find that, at least in our models, the local Δν is an at least as good and mostly better proxy for both the asymptotic spacing and the large separation scaled from the model density than the average Δν. Finally, we investigate the signature of the evolutionary stage on δν02 and quantify the mass dependency of this seismic parameter.
Key words: stars: late-type / stars: oscillations / stars: fundamental parameters / stars: interiors
© ESO, 2012
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