author={Ahmed Grigahc{\`e}ne and Victoria Antoci and Luis A. Balona and G. Catanzaro and Jadwiga Daszyńska-Daszkiewicz and Joyce A. Guzik and Gerald Handler and G Houdek and Donald W. Kurtz and Marcella Marconi and M{\'a}rio J. P. F. G. Monteiro and Andr{\'e}s Moya and Vincenzo Ripepi and J. C. Su{\'a}rez and Katrien Uytterhoeven and William J. Borucki and Timothy M. Brown and J{\o}rgen Christensen-Dalsgaard and Ronald L. Gilliland and Jon M. Jenkins and Hans Kjeldsen and David G. Koch and Stefano Bernabei and Paul Andrew Bradley and Michel Breger and Marcella Di Criscienzo and M-A. Dupret and R. A. Garc{\'i}a and A. Garc{\'i}a Hern{\'a}ndez and Jason Jackiewicz and Andreas M. Kaiser and Holger Lehmann and S. Marin-Ruiz and Ph. Mathias and Joanna Molenda–Żakowicz and J. M. Nemec and Janos Nuspl and Margit Papar{\'o} and Markus Roth and R{\'o}bert Szab{\'o} and Marian Doru Suran and Rita Ventura},
  journal={The Astrophysical Journal},
Observations of the pulsations of stars can be used to infer their interior structure and test theoretical models. The main-sequence γ Doradus (Dor) and δ Scuti (Sct) stars with masses 1.2-2.5 M ☉ are particularly useful for these studies. The γ 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 δ Sct stars pulsate in low-order g- and p-modes with periods of order 2 hr, driven by the κ mechanism… 

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