On constructing seismic models of the Sun.

Details On constructing seismic models of the Sun. On constructing seismic models of the Sun.

Jan 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996a%26a...305..631b&link_type=abstract

Astronomy and Astrophysics, v.305, p.631

Astronomy and Astrophysics

Astrophysics

18

Sun: Oscillations, Sun: Interior

Scientific paper

Observed p-mode frequencies have been extensively used to determine the the Sun's radial structure. The results of such inversions are often called "seismic models" of the Sun. In this work we investigate whether one can in fact construct models that match the measured solar frequencies to within observational errors. We invert linearized equations, relating frequency differences between the Sun and a reference model to differences in their structure, using a Regularized Least Squares (RLS) technique with second derivative smoothing. As a test, we first invert frequencies from test models. Random noise is added to these to simulate the observers' quoted errors for solar data. We investigate how the goodness of fit to the data, and the acceptability of the solution, depend upon the number of spline knots in the solution functions and upon the amount of smoothing used. With this artificial data, we can obtain a chi-squared per degree of freedom (χnu_^2^) of order unity even when the differences between the reference and test models are quite large. In contrast, using the most widely used compilation of observed solar frequencies, we are unable to get the value of χnu_^2^ close to one. Replacing the low degree data with recent data from the BISON network, and omitting frequencies determined by the ridge-fitting method (which could be more susceptible to systematic error), the value χnu_^2^ can be reduced substantially. We discuss possible causes for the small remaining excess in χnu_^2^.

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