Non linear regularization for helioseismic inversions. Application for the study of the solar tachocline

Details Non linear regularization for helioseismic inversions. Application for the study of the solar tachocline Non linear regularization for helioseismic inversions. Application for the study of the solar tachocline

1999-01-11

arxiv.org/abs/astro-ph/9901112v1

Astronomy and Astrophysics

Astrophysics

12 pages, 9 figures, accepted by A&A January 7th 1999, postscript available at http://www.obs-nice.fr/corbard/corbard_prp.html

Scientific paper

Inversions of rotational splittings have shown that there exists at the base of the solar convection zone a region called the tachocline in which high radial gradients of the rotation rate occur. The usual linear regularization methods tend to smooth out any high gradients in the solution, and may not be appropriate for the study of this zone. In this paper we use, in the helioseismic context of rotation inversions, regularization methods that have been developed for edge-preserving regularization in computed imaging. It is shown from Monte-Carlo simulations that this approach can lead directly to results similar to those reached by linear inversions which however required some assumptions on the shape of the transition in order to be deconvolved. The application of this method to LOWL data leads to a very thin tachocline. From the discussions on the parameters entering the inversion and the Monte-Carlo simulations, our conclusion is that the tachocline width is very likely below 0.05R_sun which lowers our previous estimate of 0.05+/- 0.03R_sun obtained from the same dataset (Corbard et al. 1998).

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