Two-scale mass-flux closure models for turbulence: p-mode amplitudes in solar-like stars

Details Two-scale mass-flux closure models for turbulence: p-mode amplitudes in solar-like stars Two-scale mass-flux closure models for turbulence: p-mode amplitudes in solar-like stars

Jun 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007coast.150..153b&link_type=abstract

Communications in Astroseismology, Vol. 150, p.153

Astronomy and Astrophysics

Astronomy

Scientific paper

A new closure model has been developed, which takes into account both the skewness of the velocity distribution induced by the presence of two flows in the convection zone, and the effects of turbulence onto each flow (Belkacem et al. 2006a). Applied to the formalism of p-mode excitation, it has been possible to validate this theoretical model by a comparison with the observational excitation rates in the solar case using GOLF data (see Belkacem et al. 2006b). The next step is to consider α Cen A for which observations of the mode-damping rates are available.

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