Volume 593, September 2016
|Number of page(s)||13|
|Section||Stellar structure and evolution|
|Published online||04 October 2016|
Interior rotation of a sample of γ Doradus stars from ensemble modelling of their gravity-mode period spacings⋆
1 Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D 3001 Leuven Belgium
2 Department of Astrophysics, IMAPP, Radboud University Nijmegen, PO Box 9010, 6500 GL Nijmegen, The Netherlands
Received: 31 March 2016
Accepted: 3 July 2016
Context. Gamma Doradus stars (hereafter γ Dor stars) are known to exhibit gravity- and/or gravito-intertial modes that probe the inner stellar region near the convective core boundary. The non-equidistant spacing of the pulsation periods is an observational signature of the stellar evolutions and current internal structure and is heavily influenced by rotation.
Aims. We aim to constrain the near-core rotation rates for a sample of γ Dor stars for which we have detected period spacing patterns.
Methods. We combined the asymptotic period spacing with the traditional approximation of stellar pulsation to fit the observed period spacing patterns using χ2-optimisation. The method was applied to the observed period spacing patterns of a sample of stars and used for ensemble modelling.
Results. For the majority of stars with an observed period spacing pattern we successfully determined the rotation rates and the asymptotic period spacing values, although the uncertainty margins on the latter were typically large. This also resulted directly in the identification of the modes that correspond to the detected pulsation frequencies, which for most stars were prograde dipole gravity and gravito-inertial modes. The majority of the observed retrograde modes were found to be Rossby modes. We also discuss the limitations of the method that are due to the neglect of the centrifugal force and the incomplete treatment of the Coriolis force.
Conclusions. Despite its current limitations, the proposed method was successful to derive the rotation rates and to identify the modes from the observed period spacing patterns. It forms the first step towards detailed seismic modelling based on observed period spacing patterns of moderately to rapidly rotating γDor stars.
Key words: asteroseismology / methods: data analysis / stars: fundamental parameters / stars: variables: general / stars: oscillations
Based on data gathered with the NASA Discovery mission Kepler and the HERMES spectrograph, which is installed at the Mercator Telescope, operated on the island of La Palma by the Flemish Community at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias, and supported by the Fund for Scientific Research of Flanders (FWO), Belgium, the Research Council of KU Leuven, Belgium, the Fonds National de la Recherche Scientifique (F.R.S.-FNRS), Belgium, the Royal Observatory of Belgium, the Observatoire de Genève, Switzerland, and the Thüringer Landessternwarte Tautenburg, Germany.
© ESO, 2016
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