On Dissipation inside Turbulent Convection Zones from 3D Simulations of Solar Convection

Details On Dissipation inside Turbulent Convection Zones from 3D Simulations of Solar Convection On Dissipation inside Turbulent Convection Zones from 3D Simulations of Solar Convection

2006-07-03

arxiv.org/abs/astro-ph/0607016v1

Astrophys.J.655:1166-1171,2007

Astronomy and Astrophysics

Astrophysics

13 pages, 4 figures

Scientific paper

10.1086/507937

The development of 2D and 3D simulations of solar convection has lead to a picture of convection quite unlike the usually assumed Kolmogorov spectrum turbulent flow. We investigate the impact of this changed structure on the dissipation properties of the convection zone, parametrized by an effective viscosity coefficient. We use an expansion treatment developed by Goodman & Oh 1997, applied to a numerical model of solar convection (Robinson et al. 2003) to calculate an effective viscosity as a function of frequency and compare this to currently existing prescriptions based on the assumption of Kolmogorov turbulence (Zahn 1966, Goldreich & Keeley 1977). The results match quite closely a linear scaling with period, even though this same formalism applied to a Kolmogorov spectrum of eddies gives a scaling with power-law index of 5/3.

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