Astronomy and Astrophysics – Astronomy
Scientific paper
Jun 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994japa...15..143b&link_type=abstract
Journal of Astrophysics and Astronomy, vol. 15, no. 2, p. 143-156
Astronomy and Astrophysics
Astronomy
29
Magnetohydrodynamics, Solar Convection (Astronomy), Solar Oscillations, Stellar Models, Differential Equations, Helium, Mixing Length Flow Theory, Solar Interior, Temperature Gradients
Scientific paper
An attempt is made to infer the structure of the solar convection zone from observed p-mode frequencies of solar oscillations. The differential asymptotic inversion technique is used to fine the sound speed in the solar envelope. It is found that envelope models which use the Canuto-Mazzitelli (CM) formulation for calculating the convective flux give significantly better agreement with observations than models constructed using the mixing length formalism. This inference can be drawn from both the scaled frequency differences and the sound speed difference. The sound speed in the CM envelope model is within 0.2% of that in the sun except in the region with r greater than 0.99 solar radius. The envelope models are extended below the convection zone, to find some evidence for the gravitational settling of helium beneath the base of the convection zone. It turns out that for models with a steep composition gradient below the convection zone, the convection zone depth has to be increased by about 6 Mm in order to get agreement with helioseismic observartions.
Antia H. M.
Basu Sarbani
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