Other
Scientific paper
Oct 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...285..386h&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 285, Oct. 1, 1984, p. 386-399. Research supported by the U.S. Department of
Other
5
Atmospheric Circulation, Radiative Transfer, Solar Atmosphere, Solar Oscillations, Stellar Envelopes, Asymptotic Methods, Chromosphere, Eddington Approximation, Photosphere, Stefan-Boltzmann Law, Wave Equations
Scientific paper
The theoretical waveform for an oscillation in the solar atmosphere depends on the treatment of radiative transfer. A semiempirical model for the solar atmosphere was used to study the effects of three factors on the properties of the oscillations in the photosphere and the low chromosphere. These factors are the nonlocal character of the radiation field, deviations from radiative equilibrium, and the nongray opacity. For radial long-period oscillations within the photosphere, the fractional change in temperature is ˜ 1O3 times as large as the fractional change in radius when these effects are included. This large temperature perturbation in the causal solution is due to the presence of thermal solutions that have been ignored in the traditional treatment of the nonadiabaticity. The thermal solutions arise in the improved treatment of the nonadiabaticity of the damping of oscillations in the solar atmosphere. That the temperature perturbations show such a marked sensitivity to these effects suggests that a new probe may be available for the static properties of the solar atmosphere. However, a more immediate consequence is the resolution of a long-standing problem in the study of solar oscillations: the inconsistency between the interpretation of the SCLERA diameter measurements and the Doppler shift measurements of other observers.
Hill Adrian H.
Logan Jerry D.
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