Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21361205p&link_type=abstract
American Astronomical Society, AAS Meeting #213, #612.05
Astronomy and Astrophysics
Astrophysics
Scientific paper
The current understanding of the turbulent dissipation in stellar convective zones is based on the assumption that the turbulence follows Kolmogorov scaling. This assumption is valid for some cases in which the time frequency of the external shear is high (e.g. solar p-modes). However, for many cases of astrophysical interest (e.g. binary orbits, stellar pulsations e.t.c.) the timescales of interest lie outside the regime of applicability of Kolmogorov scaling.
We present direct calculations of the dissipation efficiency of the turbulent convective flow in this regime using simulations of anelastic convection with external forcing. We show that the effects of the turbulent flow are well represented by an effective viscosity coefficient and we provide the values of the effective viscosity as a function of the perturbation frequency. In addition we justify a perturbative method for finding the effective viscosity (proposed by Goodman and Oh 1997) and apply it to actual simulations of the surface convective zones of low mass stars.
Barranco Joe
Demarque Pierre
Penev Kaloyan
Robinson Frank
Sasselov Dimitar D.
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