Asymmetries of solar oscillation line profiles

Details Asymmetries of solar oscillation line profiles Asymmetries of solar oscillation line profiles

Jun 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...410..829d&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 410, no. 2, p. 829-836.

Astronomy and Astrophysics

Astrophysics

136

Line Spectra, Power Spectra, Solar Oscillations, Solar Spectra, Spectrum Analysis, Symmetry, Fabry-Perot Interferometers, P Waves, Phase Shift

Scientific paper

Asymmetries of the power spectral line profiles of solar global p-modes are detected in full-disk intensity observations of the Ca II K Fraunhofer line. The asymmetry is a strong function of temporal frequency being strongest at the lowest frequencies observed and vanishing near the peak of the power distribution. The variation with spherical harmonic degree is small. The asymmetry is interpreted in terms of a model in which the solar oscillation cavity is compared to a Fabry-Perot interferometer with the source slightly outside the cavity. A phase difference between an outward direct wave and a corresponding inward wave that passes through the cavity gives rise to the asymmetry. The asymmetry is different in velocity and intensity observations. Neglecting the asymmetry when modeling the power spectrum can lead to systematic errors in the measurement of mode frequencies of as much as 10 exp -4 of the mode frequency. The present observations and interpretation locate the source of the oscillations to be approximately 60 km beneath the photosphere, the shallowest position suggested to date.

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