Seismic diagnostics on stellar convection treatment from oscillation amplitudes of p-modes

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dc.creatorSamadi, R.
dc.creatorGoupil, M. J.
dc.creatorLebreton, Y.
dc.creatorNordlund, A.
dc.creatorBaudin, F.
dc.date2002-10-01
dc.date.accessioned2026-07-07T02:05:32Z
dc.date.available2026-07-07T02:05:32Z
dc.descriptionThe excitation rate P of solar p-modes is computed with a model of stochatic 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 ~9 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 (1Mo < M < 2Mo). Differences in the values of P_max 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.
dc.description4 pages, 1 figure, proceedings of the conference "Asteroseismology Across the HR Diagram" held in Porto (Portugal) in July 2002, to be published by Kluwer as an issue of the Astrophysics and Space Science Journal
dc.identifierhttps://arxiv.org/abs/astro-ph/0210036
dc.identifierhttp://arxiv.org/abs/astro-ph/0210036
dc.identifierAstrophys.Space Sci. 284 (2003) 221-224
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/5130
dc.subjectAstrophysics
dc.titleSeismic diagnostics on stellar convection treatment from oscillation amplitudes of p-modes
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