Astronomy and Astrophysics – Astronomy
Scientific paper
May 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006apj...643..426d&link_type=abstract
The Astrophysical Journal, Volume 643, Issue 1, pp. 426-437.
Astronomy and Astrophysics
Astronomy
12
Convection, Stars: Evolution
Scientific paper
We present in this paper an anisotropic nonlocal theory of stellar convection. Following the idea of Rotta, we propose that the correlation of turbulent pressure and velocity gradient tends to make the turbulent velocity isotropic, and we further introduce a convection parameter c3 to measure the strength of such isotropization. By using such a theory, the structure of the solar convection zone is calculated. Our calculation shows that the radial component dominates in the convectively unstable zone, in which the ratio between the radial component and the horizontal component is w2r/w2h=(3+c3)/2c3. In the upper overshooting zone, turbulent velocity is almost isotropic (w2r/w2h~0.5) and is independent of c3, while in the lower overshooting zone, w2r/w2h<=0.5, and it tends to decrease as c3 decreases. We also studied the effects of anisotropic convection on the structure and evolution of stars. It is shown that the anisotropy hardly affects the temperature and pressure structure of stars. However, the anisotropy increases with the decrease of c3; therefore, the effect of overshooting decreases. Thus, the effects of anisotropy of turbulent convection on stellar evolution cannot be neglected.
Chan Kwan-Leung
Deng Licai
Xiong Da-Run
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