Line Asymmetry of Solarp‐Modes: Properties of Acoustic Sources

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Abstract
The observed solar p-mode velocity power spectra are compared with theoretically calculated power spectra over a range of mode degree and frequency. The shape of the theoretical power spectra depends on the depth of acoustic sources responsible for the excitation of p-modes and also on the multipole nature of the source. We vary the source depth to obtain the best fit to the observed spectra. We find that quadrupole acoustic sources provide a good fit to the observed spectra provided that the sources are located between 700 and 1050 km below the top of the convection zone. The dipole sources give a good fit for a significantly shallower source, with a source depth of between 120 and 350 km. The main uncertainty in the determination of depth arises because of poor knowledge of the nature of power leakages from modes with adjacent degrees and the background in the observed spectra.
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