Modelling the solar oscillation time series by a randomly excited oscillator

Details Modelling the solar oscillation time series by a randomly excited oscillator Modelling the solar oscillation time series by a randomly excited oscillator

Dec 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988esasp.286..673l&link_type=abstract

In ESA, Seismology of the Sun and Sun-Like Stars p 673-676 (SEE N89-25819 19-92)

Computer Science

3

Parameter Identification, Solar Cycles, Solar Oscillations, Spectrum Analysis, Time Series Analysis, Curve Fitting, Fourier Analysis, Power Spectra, Random Processes

Scientific paper

Artificial full solar disk data is used to determine the parameters of a randomly excited oscillator by comparison with observation data. The artificial signal is used to test the methods of analysis used for the precise determination of mode frequencies, amplitudes and linewidths. The reliability of centroid measurements made by barycenter, Lorentzian fit, and Gaussian fit, with and without background noise was tested. Methods for line width measurements were also assessed. For the determination of the central frequency, taking the highest peak is not the best choice. Fitting a Lorentz curve is better. For line width the Gaussian fit seems to be better defined, but the Lorentzian one is preferred, since it finds a better value for the actual width. However, since sometimes the fitting procedure yields erroneously to a very small linewidth, care should be taken, especially when the number of realizations is not high enough to show clearly the bimodal distribution. Once this distribution is obtained, various techniques could be applied to prevent the fitting procedure reaching the absolute minimum of residuals.

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