Open AccessNon‐linear inversion for the hydrostatic structure of the solar interior
Author(s) -
Marchenkov Konstantin,
Roxburgh Ian,
Vorontsov Sergei
Publication year - 2000
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1046/j.1365-8711.2000.03059.x
Subject(s) - physics , convection zone , inversion (geology) , convection , computational physics , hydrostatic equilibrium , helioseismology , inverse transform sampling , inverse , geophysics , mathematical analysis , astrophysics , optics , mechanics , geometry , magnetic field , geology , surface wave , astronomy , mathematics , paleontology , structural basin , quantum mechanics
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.