Volume 435, Number 3, June I 2005
|Page(s)||927 - 939|
|Section||Stellar structure and evolution|
|Published online||13 May 2005|
II. Excitation and stabilization mechanisms in δ Sct and γ Dor stars
Instituto de Astrofísica de Andalucía-CSIC, Apartado 3004, 18080 Granada, Spain e-mail: email@example.com
2 Institut d'Astrophysique et de Géophysique de l'Université de Liè ge, Belgium
Accepted: 23 January 2005
We apply here the Time Dependent Convection (TDC) treatment presented in our earlier paper in this series to the study of δ Sct and γ Dor pulsating stars. Stabilization of the δ Sct p-modes at the red edge of the Instability Strip (IS) and the driving of the γ Dor g-modes are explained by our models. Theoretical IS obtained with different values of the Mixing Length (ML) parameter α are compared to observations and a good agreement is obtained for α between 1.8 and 2. The influence of each term of our TDC treatment (perturbation of convective flux, turbulent pressure, and turbulent kinetic energy dissipation) on the eigenfrequencies and on the driving and damping mechanisms is investigated. Finally, we show that our TDC models predict the likely existence of hybrid stars with both δ Sct p-modes and γ Dor g-modes oscillations.
Key words: stars: oscillations / convection / stars: interiors / stars: variables: δ Sct / stars: variables: general
© ESO, 2005
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.