Driving the Gravity-Mode Pulsations in γ Doradus Variables

By J. Guzik, A. B. Kaye, P. Bradley, A. N. Cox, C. Neuforge. 2000

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Theoretical instability strips for δ Scuti and γ Doradus stars (2004, background): “In both TDC and FC models, the main driving occurs at the base of the convective envelope (in agreement with Guzik et al. 2000).”
KOI-54: THE KEPLER DISCOVERY OF TIDALLY EXCITED PULSATIONS AND BRIGHTENINGS IN A HIGHLY ECCENTRIC BINARY (2011, methodology): “Thus, we calculated the ℓ= 2, m=0 g-mode eigensolutions for each of these stars using the procedure and nonadiabatic non-radial pulsation code of Pesnell (1990) as reported in Guzik et al. (2000).”
The Orbit and Pulsation Periods of the γ Doradus Variable HR 6844 (V2502 Ophiuchi) (2003, background): “Guzik et al. (2000) developed the first models of a driving mechanism for these gravitymode pulsations.”
Probing the properties of convective cores through g modes : high-order g modes in SPB and γ Doradus stars (2008, background): “The former are main-sequence stars with masses around 1.5 M (see e.g. Guzik et al. 2000) that show both photometric and line profile variations.”
HYBRID γ DORADUS–δ SCUTI PULSATORS: NEW INSIGHTS INTO THE PHYSICS OF THE OSCILLATIONS FROM KEPLER OBSERVATIONS (2010, methodology): “Guzik et al. (2000), using frozen-convection models, and Dupret et al. (2005, 2006), using time-dependent convection (Grigahcène et al. 2005), have shown that the position of the convective envelope base is the key to driving γ Dor g modes.”