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Breger, M. Di Criscienzo, M.D. Suran, M. J. P. F. G. Monteiro, M. Marconi, M. Paparo, M. Roth, P. Bradley, P. Mathias, R. A. Garcia, R. L. Gilliland, R. Szabo, R. Ventura, S. Bernabei, S. Marin-Ruiz, T. M. Brown, V. Antoci, V. Ripepi, W. J. Borucki","submitted_at":"2010-01-05T19:20:53Z","abstract_excerpt":"Observations of the pulsations of stars can be used to infer their interior structure and test theoretical models. The main sequence $\\gamma$ Doradus (Dor) and $\\delta$ Scuti (Sct) stars with masses 1.2-2.5 $M_{\\sun}$ are particularly useful for these studies. The $\\gamma$ Dor stars pulsate in high-order $g$ modes with periods of order 1 day, driven by convective blocking at the base of their envelope convection zone. The $\\delta$ Sct stars pulsate in low-order $g$ and $p$ modes with periods of order 2 hours, driven by the $\\kappa$ mechanism operating in the Heii ionization zone. 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