The seismic radius of the Sun, and structure inversions

Computer Science – Sound

Scientific paper

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Solar Radius, Inversion, P-Modes

Scientific paper

It is known (Schou et al., 1997; Antia, 1998) that the effective radius of the Sun determined by f-mode frequencies is different by a few hundredths per cent from the photospheric radius determined by direct photometric measurement (Brown and Christensen-Dalsgaard 1998). It is fair to say that we still do not fully comprehend the implications of the difference, save that the two radii are rather different quantities: the radius inferred from f-mode frequencies is determined by the location of the maximum in the f-mode energy (Gough, 1993), whereas the photospheric radius is determined by extrapolation to some prescribed optical depth from a fiducial point in the limb-darkening function using a theoretical solar model. Both depend in particular on the structure of the upper superadiabatic convective boundary layer, the physics of which is not well understood. In this report we attempt to shed some light on the difference by determining a seismic radius from p-mode frequencies; the outcome depends predominantly on the variation of sound speed, and it is consistent with the f-mode value (Takata and Gough 2001). By considering the mathematical structure of an inversion process that does not explicitly distinguish f modes from p modes, we offer an interpretation of the seismic radius. This interpretation has led us to revise the method by which we carry out structure inversions.

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