Influence of local treatments of convection upon solar p mode excitation rates

Abstract

We compute the rates P at which acoustic energy is injected into the solar radial p modes for several solar models. The solar models are computed with two different local treatments of convection: the classical mixing-length theory (MLT hereafter) and Canuto et al (1996)'s formulation (CGM hereafter). Among the models investigated here, our best models reproduce both the solar radius and the solar luminosity at solar age and the observed Balmer line profiles. For the MLT treatment, the rates P do depend significantly on the properties of the atmosphere whereas for the CGM's treatment the dependence of P on the properties of the atmosphere is found smaller than the error bars attached to the seismic measurements. The excitation rates P for modes associated with the MLT models are significantly underestimated compared with the solar seismic constraints. The CGM models yield values for P closer to the seismic data than the MLT models. We conclude that the solar p-mode excitation rates provide valuable constraints and according to the present investigation clearly favor the CGM treatment with respect to the MLT, although neither of them yields values of P as close to the observations as recently found for 3D numerical simulations.

arXiv comment11 pages, 7 figures, accepted for publication in Astronomy & Astrophysics

References in corpus (12)

• Line formation in solar granulation: IV. [O I], OI and OH lines and the photospheric O abundance
• Helioseismological Implications of Recent Solar Abundance Determinations
• Stellar Turbulent Convection: A Selfconsistent Model
• Constraining solar abundances using helioseismology
• Solar Oscillations and Convection: II. Excitation of Radial Oscillations
• New grids of ATLAS9 atmospheres I: Influence of convection treatments on model structure and on observable quantities
• Excitation of stellar p-modes by turbulent convection: 1. Theoretical formulation
• The discrepancy between solar abundances and helioseismology
• Numerical constraints on the model of stochastic excitation of solar-type oscillations
• A-star envelopes: a test of local and non-local models of convection
• Numerical 3D constraints on convective eddy time-correlations : consequences for stochastic excitation of solar p modes
• Convection in the atmospheres and envelopes of Pre-Main Sequence stars

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