Physics
Scientific paper
Dec 1988
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988esasp.286...17b&link_type=abstract
In ESA, Seismology of the Sun and Sun-Like Stars p 17-20 (SEE N89-25819 19-92)
Physics
3
Line Spectra, P Waves, Photosphere, Solar Oscillations, Helioseismology, Radiative Transfer, Solar Physics
Scientific paper
Measurements show that the 5 m oscillations have different amplitudes in the opposite flanks of several photospheric lines. This effect can be suitably described by giving the (blue wing)/(red wing) ratio of the rms wavelength shift at any given level of residual intensity. The main cause is radiative damping, which produces a depth dependent phase difference between the velocity and the thermodynamical (temperature and pressure) perturbations within the line forming region. Synthetic profiles of the FeI 6301.5 A line, obtained by numerical solution of the time independent radiative transfer equation in the oscillating atmosphere (quasi-static radiation field approximation) show that agreement between observed and computed profiles can be achieved. The consequences of this effect (which is also dependent on the magnetic flux concentration) on the diagnostic properties of line profiles are discussed.
Bertello Luca
Caccin Bruno
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