Hostname: page-component-788cddb947-2s2w2 Total loading time: 0 Render date: 2024-10-14T03:27:42.675Z Has data issue: false hasContentIssue false
  • English
  • Français

Convective Overshooting to Drive g-Modes in γ Dor Stars

Published online by Cambridge University Press:  13 May 2016

Y. Li
Y. Li*
Affiliation:
Yunnan Observatory, NAOCAS, P.O. Box 110, Kunming, 650011 China

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

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.

Type
Session I: Global Structure and Evolution of the Solar Interior
Information
Symposium - International Astronomical Union , Volume 203: Recent Insights into the Physics of the Sun and Heliosphere: Highlights from Soho and Other Space Missions , 2001 , pp. 62 - 65
Copyright
Copyright © Astronomical Society of the Pacific 2001 

References

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