Modeling the γ Doradus Instability Strip: Preliminary Results

Details Modeling the γ Doradus Instability Strip: Preliminary Results Modeling the γ Doradus Instability Strip: Preliminary Results

Dec 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001aas...199.9005w&link_type=abstract

American Astronomical Society, 199th AAS Meeting, #90.05; Bulletin of the American Astronomical Society, Vol. 33, p.1436

Astronomy and Astrophysics

Astronomy

Scientific paper

The γ Doradus stars are a newly discovered class of gravity-mode pulsators that lie just beyond the red edge of the δ Scuti instability strip. We present preliminary results of calculations of models between 1.0 and 2.5 Msun, Z=0.02, l= 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 γ Doradus instability strip. In addition, we compare these calculational results with previously-published observational results.

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