Poster
A. Grigahcène, J. Pascual, J. Gutiérrez-Soto, K. Uytterhoeven, L. A. Balona, R. A. Garcia, S. Martín-Ruiz, E. Niemczura, A. Moya Bedón, L. Fox-Machado, J.-C. Suárez, H. Lehmann, O. L. Creevey, S. Benatti, A. García Hernández, P. J. Amado, M. J. P. F. G. Monteiro, J. A. Guzik
Abstract
γ Doradus pulsators show high-order gravity modes with periods ranging from 0.3 to 3 days. Ground based observations of these stars are often complicated by the aliasing of one day and the very low level of amplitudes. However, the Kepler space mission, providing high-quality light curves of unprecedented length and accuracy, promises a breakthrough in the study of such variable stars. Not only do the Kepler data solve aliasing and photometric stability problems encountered in ground-based photometric campaigns, the wealth of detected frequencies found in γ Dor stars will also help to overcome difficulties with mode identification, as asymptotic analysis techniques can be applied. We present the preliminary results of a set of pure γ Dor candidates. We aim at studying their pulsational characteristics, mainly their frequency range and amplitudes, taking into account their positions in the HR diagram.
Third Kepler Asteroseismology Workshop: 'Kepler Asteroseismology in Action'
Aarhus, Denmark
2010 June
