Astronomy and Astrophysics – Astronomy
Scientific paper
Jul 2000
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000apj...538..346l&link_type=abstract
The Astrophysical Journal, Volume 538, Issue 1, pp. 346-362.
Astronomy and Astrophysics
Astronomy
1
Stars: Variables: Cepheids, Stars: Variables: Δ Scuti, Instabilities, Stars: Interiors, Stars: Oscillations
Scientific paper
By using four different frozen-convection approximations, we investigate nonadiabatic radial pulsations for a 9 Msolar and a 2 Msolar stellar model, which represent, respectively, the Cepheid and δ Scuti variables, and we compare the characteristics of the pulsations. We find that the periods of the pulsation modes can differ as much as 6% for the 9 Msolar model and a small amount for the 2 Msolar model. The locations of the pulsation instability strips produced by the four frozen-convection approximations are significantly different from each other, as well as the eigenfunctions and work integrals. It is found that the approximation L'C=0 restrains the driving feature at the bottom of the convection zone in the quasi-adiabatic stellar interior and then gives rise to the red edge of the instability strip, while the approximations δFC=0 and δLC=0 result in the correct locations of the blue edges of the instability strips that are in good agreement with the observations. We conclude that each of the four frozen-convection approximations may describe some aspects of the convection-pulsation interaction, but none of them can be a complete solution of the problem. Based on considerations of the timescales of the pulsation and response time of the convection, we suggest that a combination of proper frozen-convection approximations may be a good measure of the nonadiabatic stellar pulsations.
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