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Solar-like oscillations in subgiant and red-giant stars: mixed modes

Published online by Cambridge University Press:  18 February 2014

S. Hekker  and
A. Mazumdar
S. Hekker
Affiliation:
Max Planck Institute for Solar System Research, Katlenburg-Lindau, Germany email: [email protected] Astronomical Institute “Anton Pannekoek”, University of Amsterdam, Amsterdam, the Netherlands
A. Mazumdar
Affiliation:
Homi Bhabha Centre for Science Education, TIFR, Mumbai, India
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Abstract

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Thanks to significant improvements in high-resolution spectrographs and the launch of dedicated space missions MOST, CoRoT and Kepler, the number of subgiants and red-giant stars with detected oscillations has increased significantly over the last decade. The amount of detail that can now be resolved in the oscillation patterns does allow for in-depth investigations of the internal structures of these stars. One phenomenon that plays an important role in such studies are mixed modes. These are modes that carry information of the inner radiative region as well as from the convective outer part of the star allowing to probe different depths of the stars.

Here, we describe mixed modes and highlight some recent results obtained using mixed modes observed in subgiants and red-giant stars.

Keywords

stars: oscillations (including pulsations)stars: evolution
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Symposium S301: Precision Asteroseismology , August 2013 , pp. 325 - 331
Copyright
Copyright © International Astronomical Union 2014 

References

Aerts, C., Christensen-Dalsgaard, J., & Kurtz, D. W., 2010, Asteroseismology, Astronomy and Astrophysics Library (Springer Science+Business Media B.V.)Google Scholar
Aizenman, M., Smeyers, P., & Weigert, A. 1977, A&A, 58, 41Google Scholar
Beck, P. G., Bedding, T. R., Mosser, B., et al. 2011, Science, 332, 205Google Scholar
Beck, P. G., Montalbán, J., Kallinger, T., et al. 2012, Nature, 481, 55Google Scholar
Bedding, T. R., Mosser, B., Huber, D., et al. 2011, Nature, 471, 608CrossRefGoogle Scholar
Benomar, O., Bedding, T. R., Mosser, B., et al. 2013, ApJ, 767, 158Google Scholar
Chaplin, W. J. & Miglio, A. 2013, ARAA, 51, 353Google Scholar
Christensen-Dalsgaard, J. 2011, arXiv: 1106.5946Google Scholar
Deheuvels, S., García, R. A., Chaplin, W. J., et al. 2012, ApJ, 756, 19Google Scholar
Deheuvels, S. & Michel, E. 2010, Ap&SS, 328, 259Google Scholar
Dupret, M.-A., Belkacem, K., Samadi, R., et al. 2009, A&A, 506, 57Google Scholar
Goldreich, P. & Keeley, D. A. 1977, ApJ, 212, 243Google Scholar
Goldreich, P. & Kumar, P. 1988, ApJ, 326, 462Google Scholar
Gough, D. O. 1986, Highlights of Astronomy, 7, 283Google Scholar
Hekker, S. 2013, Adv. Sp. Res., 52, 1581Google Scholar
Karoff, C. 2007, MNRAS, 381, 1001CrossRefGoogle Scholar
Mosser, B., Barban, C., Montalbán, J., et al. 2011, A&A, 532, A86Google Scholar
Mosser, B., Goupil, M. J., Belkacem, K., et al. 2012, A&A, 548, A10Google Scholar
Tassoul, M. 1980, ApJS, 43, 469Google Scholar