Non-linear inversion for the hydrostatic structure of the solar interior

Details Non-linear inversion for the hydrostatic structure of the solar interior Non-linear inversion for the hydrostatic structure of the solar interior

Feb 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000mnras.312...39m&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 312, Issue 1, pp. 39-50.

Astronomy and Astrophysics

Astronomy

10

Sun: Interior, Sun: Oscillations

Scientific paper

We present the results of a non-linear inverse analysis for the hydrostatic, spherically symmetric component of the solar internal structure using the observed p-mode frequencies. The iterative non-linear inversion technique used here is based on the succesive Born approximation description of solar p-modes developed by Roxburgh & Vorontsov. This description can give a high resolution of regions of rapid variation of seismic parameters with depth (e.g., the base of the convection zone), and accounts accurately for the strong influence of gravity perturbations on low-degree modes which penetrate deep into the solar core. The inversion procedure is non-linear; the eigenfrequency equation obtained from the Born approximation is solved by iteration. The particular target of our inverse analysis is to achieve the highest possible resolution of the region near the base of the solar convection zone, searching for possible signatures of penetrative convection, element diffusion and/or strong magnetic fields. The results of the global inversion obtained with solar p-mode frequencies provided by the recent high-quality observational data (GONG, SOI/MDI, GOLF) are presented and discussed.

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