Estimation of turbulent diffusivity with direct numerical simulation of stellar convection

Details Estimation of turbulent diffusivity with direct numerical simulation of stellar convection Estimation of turbulent diffusivity with direct numerical simulation of stellar convection

2012-04-17

arxiv.org/abs/1204.3695v1

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

18 pages, 4 figures, 1 table, accepted to ApJL

Scientific paper

We investigate the value of horizontal turbulent diffusivity {\eta} by numerical calculation of thermal convection. In this study, we introduce a new method whereby the turbulent diffusivity is estimated by monitoring the time devel- opment of the passive scalar, which is initially distributed in a given Gaussian function with a spatial scale d0. Our conclusions are as follows: (1) Assuming the relation {\eta} = Lcvrms/3 where vrms is the RMS velocity, the characteristic length Lc is restricted by the shortest one among the pressure (density) scale height and the region depth. (2) The value of turbulent diffusivity becomes greater with the larger initial distribution scale d0. (3) The approximation of turbulent diffusion holds better when the ratio of the initial distribution scale d0 to the characteristic length Lc is larger.

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