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Nonlinear Inversion for the Hydrostatic Structure of the Solar Interior

Published online by Cambridge University Press:  08 February 2017

K.I. Marchenkov ,
I.W. Roxburgh  and
S.V. Vorontsov
K.I. Marchenkov
Affiliation:
Astronomy Unit, Queen Mary College, University of London, Mile End Road, London E1 4NS, UK
I.W. Roxburgh
Affiliation:
Astronomy Unit, Queen Mary College, University of London, Mile End Road, London E1 4NS, UK
S.V. Vorontsov
Affiliation:
Astronomy Unit, Queen Mary College, University of London, Mile End Road, London E1 4NS, UK

Extract

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The technique which we use is based on the “quasi-asymptotic” description of solar p-modes developed by Roxburgh & Vorontsov (1996). As a significant improvement of the standard asymptotic analysis, this description incorporates a Born approximation to allow for a detailed treatment of the regions of rapid variation of seismic parameters with depth (base of the convection zone) and strong influence of gravity perturbations (low-degree modes which penetrate deep into the solar core).

Type
II. Solar Convection and Variation of Irradiance
Information
Symposium - International Astronomical Union , Volume 185: New Eyes to See Inside the Sun and Stars , 1998 , pp. 117 - 118
Copyright
Copyright © Kluwer 1998 

References

Christensen-Dalsgaard, J., et al.: 1996, Science 272, 1286.Google Scholar
Roxburgh, I.W., and Vorontsov, S.V.: 1996, Monthly Notices Roy. Astron. Soc. 278, 940.Google Scholar