Seismology of the solar convection zone

Basu, Sarbani ; Antia, H. M. (1994) Seismology of the solar convection zone Journal of Astrophysics and Astronomy, 15 (2). pp. 143-156. ISSN 0250-6335

PDF - Publisher Version

Official URL:

Related URL:


An attempt is made to infer the structure of the solar convection zone from observedp-mode frequencies of solar oscillations. The differential asymptotic inversion technique is used to find 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 > 0.99 R. 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 observations.

Item Type:Article
Source:Copyright of this article belongs to Indian Academy of Sciences.
Keywords:Sun: Oscillations; Convection
ID Code:12298
Deposited On:10 Nov 2010 06:33
Last Modified:16 May 2016 21:40

Repository Staff Only: item control page