Dynamical Characteristics Of Surface Convection In The Sun And A Population II Star

Details Dynamical Characteristics Of Surface Convection In The Sun And A Population II Star Dynamical Characteristics Of Surface Convection In The Sun And A Population II Star

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...208.0602b&link_type=abstract

American Astronomical Society Meeting 208, #6.02; Bulletin of the American Astronomical Society, Vol. 38, p.84

Physics

Scientific paper

We present the results of the 3 dimensional radiative hydrodynamic numerical large eddy simulations of the outer layers of stars. The goal of this study is to compare convection phenomenon of a Pop II star with the Sun. We have constructed a Pop II star of 0.7 solar mass and metallicity z=0.0004. The results are compared to a similar simulation performed for the Sun using the same detailed physics input and numerical code. The domains of simulations extend from the observable atmospheric layers in radiative equilibrium and the outer layers of the convection zones, down to a depth at which the temperature gradient exceeds the adiabatic value by only a very small amount. Each simulation has been made for 32 and 24 minutes for the Sun and a Pop II star, respectively, and the thermal and dynamical structures of each star including overshoot are explored. The vertical and horizontal sizes of granules, dominantly affected by the turbulence, are smaller in a Pop II star. These results indicate that a Pop II star has less turbulent structures than that of the Sun because of its higher density distribution and surface gravity.

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