Seismic Diagnostics on Stellar Convection Treatment from Oscillation Amplitudes of p-modes
Source: Astrophysics and Space Science, Volume 284, Number 1, 2003 , pp. 221-224(4)
The excitation rate P of solar p-modes is computed with a model of stochastic excitation which involves constraints on the averaged properties of the solar turbulence. These constraints are obtained from a 3D simulation. Resulting values for P are found ∼ 4.5 times larger than when the calculation assumes properties of turbulent convection which are derived from an 1D solar model based on Gough (1977)'s formulation of the mixing-length theory (GMLT). This difference is mainly due to the assumed values for the mean anisotropy of the velocity field in each case. Calculations based on 3D constraints bring the P maximum closer to the observational one. We also compute P for several models of intermediate mass stars (1 ≲ M ≲ 2 M⊙). Differences in the values of Pmax between models computed with the classical mixing-length theory and GMLT models are found large enough for main sequence stars to suggest that measurements of P in this mass range will be able to discriminate between different models of turbulent convection.
Document Type: Research Article
Affiliations: 1: Astronomy Unit, Queen Mary, University of London, London, UK 2: Observatoire de Paris-Meudon, Meudon, France 3: Niels Bohr Institute for Astronomy Physics and Geophysics, Copenhagen, Denmark 4: Institut d'Astrophysique Spatiale, Orsay, France
Publication date: 2003