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Convective Overshooting to Drive g-Modes in γ Dor Stars

  • Y. Li (a1)

Abstract

From considerations of kinetic energy input from turbulent convection into g-mode pulsation, we show that g-mode pulsation may obtain enough energy from the turbulence to overcome damping in the stellar interior. The development of thick convective envelope in the stellar models requires a small value of the convection parameter α = 1.2 to ensure the low mass limit of the γ Dor stars' instability strip to be in agreement with the observations.

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References

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Gautschy, A., & Löffler, W., 1996, Delta Scuti Stars Newsletter, 10, 13.
Guzik, J.A., & Swenson, F.J., 1997, ApJ, 491, 967.
Handler, G., 1999, MNRAS, 309, L19.
Kaye, A.B., Handler, G., Krisciunas, K., Poretti, E., & Zerbi, F.M., 1999, PASP, 111, 840.
Krisciunas, K., 1998, in New Eyes to See Inside the Sun and Stars, IAU Symp. 185, eds. Deubner, F.-L. et al., p.339.

Convective Overshooting to Drive g-Modes in γ Dor Stars

  • Y. Li (a1)

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