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P. B. Warner (Brigham Young University), A. B. Kaye, J. A. Guzik (Los Alamos National Laboratories), E. G. Hintz (Brigham Young University)
The \gamma Doradus stars are a newly discovered class of gravity-mode pulsators that lie just beyond the red edge of the \delta Scuti instability strip. We present preliminary results of calculations of models between 1.0 and 2.5 M\odot, Z=0.02, \ell= 1 to 4, and periods between 0.5 and 3 days. Models that predict pulsational instability with high-order g-modes and local convective timescales comparable to or longer than the pulsation period, define the \gamma Doradus instability strip. In addition, we compare these calculational results with previously-published observational results.
The author(s) of this abstract have provided an email address for comments about the abstract: phil@tardis.byu.edu