Physics
Scientific paper
Apr 1976
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976soph...47..435s&link_type=abstract
Solar Physics, vol. 47, Apr. 1976, p. 435-460.
Physics
55
Photosphere, Propagation Modes, Solar Spectra, Wave Propagation, Acoustic Propagation, Line Spectra, Magnetohydrodynamics, Phase Shift, Power Spectra, Propagation Velocity, Relaxation Time
Scientific paper
Using a 32-minute sequence of observation, brightness and velocity fluctuations in the wings of the Mg I line at 5172.7 A and the Fe II line at 5197.578 A are analyzed in terms of phase shifts and amplitude ratios. In the frequency range from 1/400 s to 1/130 s, three modes of waves are found to exist: internal gravity, evanescent, and propagating acoustic waves which appear with increasing frequency. A satisfactory agreement for velocity between observations and theory in the range of horizontal wavelengths greater than 5000 km with a theoretically local relaxation time of about 80 s to 40 s is obtained. It is shown that the Mg I line is sensitive to temperature and density fluctuations while the Fe II lines is only sensitive to temperature perturbation. For the best fit with the same local relaxation time to both lines, it is found that the density effect should be taken into account for the Mg I intensity fluctuations. The relaxation time deduced from observed intensity fluctuations seems to decrease with the period of oscillation, suggesting the presence of a dissipation process. For higher-frequency oscillations, the phase shift and the amplitude ratios are too small to be interpreted by propagating acoustic waves.
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