On the opacity change required to compensate for the revised solar composition

Abstract

Recent revisions of the determination of the solar composition have resulted in solar models in marked disagreement with helioseismic inferences. The effect of the composition change on the model is largely caused by the change in the opacity. Thus we wish to determine an intrinsic opacity change that would compensate for the revision of the composition. By comparing models computed with the old and revised composition we determine the required opacity change. Models are computed with the opacity thus modified and used as reference in helioseismic inversions to determine the difference between the solar and model sound speed. An opacity increase varying from around 30 per cent near the base of the convection zone to a few percent in the solar core results in a sound-speed profile, with the revised composition, which is essentially indistinguishable from the original solar model. As a function of the logarithm of temperature this is well represented by a simple cubic fit. The physical realism of such a change remains debatable, however.

Astron. Astrophys., in the press

References in corpus (18)

• Helioseismology and Solar Abundances
• Up-dated opacities from the Opacity Project
• Helioseismological Implications of Recent Solar Abundance Determinations
• Constraining solar abundances using helioseismology
• The photospheric solar oxygen project: I. Abundance analysis of atomic lines and influence of atmospheric models
• Standard Solar models in the Light of New Helioseismic Constraints II. Mixing Below the Convective Zone
• Photospheric Abundances: Problems, Updates, Implications
• Surprising Sun
• The Solar Heavy Element Abundances: I. Constraints from Stellar Interiors
• Solar Carbon Monoxide, Thermal Profiling, and the Abundances of C, O, and their Isotopes
• Solar internal sound speed as inferred from combined BiSON and LOWL oscillation frequencies
• Determining solar abundances using helioseismology
• Solar heavy element abundance: constraints from frequency separation ratios of low-degree p modes
• A Constraint on Z_\odot from Fits of Isochrones to the Color-Magnitude Diagram of M67
• Seismic study of the chemical composition of the solar convection zone
• The solar photospheric abundance of phosphorus: results from co5bold 3D model atmospheres
• Effects of Heavy Elements and Excited States in the Equation of State of the Solar Interior
• On the seismic age of the Sun

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