Physics
Scientific paper
May 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21431402p&link_type=abstract
American Astronomical Society, AAS Meeting #214, #314.02; Bulletin of the American Astronomical Society, Vol. 41, p.758
Physics
Scientific paper
The turbulent flow in stellar convective zones is believed to be an important dissipation mechanism for phenomena like tides and stellar pulsations. The current understanding of this dissipation is based on the assumption that the turbulence follows Kolmogorov scaling. This assumption is reasonable for external shear with high time frequency (e.g. solar p-modes). However, for many cases of astrophysical interest (e.g. binary orbits, Cepheid pulsations etc.) the relevant timescales fall outside of the inertial subrange. We present direct calculations of the turbulent dissipation derived from simulations of stratified anelastic convection with external shear built directly into the equations of motion. We show that the observed dissipation is well parametrized as an effective viscosity coefficient and we derive the values of this coefficient as a function of the forcing period and the direction and amplitude of the shear. In addition we justify a perturbative method for finding the effective viscosity (proposed by Gooman and Oh. 1997) and use it to estimate the effective viscosity in the surface convective zones of low mass stars, using fully compressible numerical simulations with realistic physics specific to such stars.
Barranco Joe
Demarque Pierre
Penev Kaloyan
Robinson Frank
Sasselov Dimitar D.
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