SEISMOLOGY OF THE SOLAR CONVECTION ZONE

BASU S ANTIA HM

S. Basu et Hm. Antia, SEISMOLOGY OF THE SOLAR CONVECTION ZONE, Journal of astrophysics and astronomy, 15(2), 1994, pp. 143-156

21

INGLESE

Article

Astronomy & Astrophysics

Journal of astrophysics and astronomy → ACNP

0250-6335

15

2

1994

143 - 156

ISI

0250-6335(1994)15:2<143:SOTSCZ>2.0.ZU;2-L

An attempt is made to infer the structure of the solar convection zone from observed p-mode frequencies of solar oscillations. The different ial asymptotic inversion technique is used to find the sound speed in the solar envelope. It is found that envelope models which use the Can uto-Mazzitelli (CM) formulation for calculating the convective flux gi ve significantly better agreement with observations than models constr ucted using the mixing length formalism. This inference can be drawn f rom both the scaled frequency differences and the sound speed differen ce. The sound speed in the CM envelope model is within 0.2% of that in the Sun except in the region with r>0.99R. The envelope models are ex tended below the convection zone, to find some evidence for the gravit ational 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 abo ut 6 Mm in order to get agreement with helioseismic observations.