ASYMMETRIES OF SOLAR OSCILLATION LINE-PROFILES

Asymmetries of the power spectral line profiles of solar global p-mode s are detected in full-disk intensity observations of the Ca II K Frau nhofer line. The asymmetry is a strong function of temporal frequency, nu, being strongest (almost-equal-to 10%) at the lowest frequencies o bserved (nu congruent-to 2 mHz) and vanishing near the peak of the pow er distribution (nu congruent-to 3.2 mHz). The variation with spherica l harmonic degree is small. The asymmetry is interpreted in terms of a model in which the solar oscillation cavity is compared to a Fabry-Pe rot interferometer with the source slightly outside the cavity. A phas e 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. Neglect ing the asymmetry when modeling the power spectrum can lead to systema tic errors in the measurement of mode frequencies of as much as 10(-4) of the mode frequency. The present observations and interpretation lo cate the source of the oscillations to be approximately 60 km beneath the photosphere, the shallowest position suggested to date.