Limits on coronal reflection using high-frequency solar oscillations

Details Limits on coronal reflection using high-frequency solar oscillations Limits on coronal reflection using high-frequency solar oscillations

Feb 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...422l..29k&link_type=abstract

Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 422, no. 1, p. L29-L32

Astronomy and Astrophysics

Astrophysics

23

Magnetic Fields, Solar Atmosphere, Solar Flux, Solar Oscillations, Solar Radio Emission, Chromosphere, Photosphere, Solar Corona, Solar Limb, Solar Wind

Scientific paper

Acoustic waves in the Sun with frequencies above about 5.3 mHz can propagate in the chromosphere. We examine imaged solar intensity data for evidence of reflection of these waves in the upper chromosphere, where the temperature increases by a large factor over a short distance. Our method is to compare the observed and theoretically derived frequency spacings between peaks in the power spectrum. We find that our theoretical frequencies provide the best fit to the data when the reflection in the upper atmosphere is eliminated. In particular, the model of Kumar (1993b), which includes the source depth, and radiative damping, in the calculation of power spectra but ignores chromospheric reflection, gives peak frequencies that are in good agreement with the observations. For acoustic waves of frequency greater than 6 mHz we put an upper limit to the reflectivity of chromosphere and corona, using our method, of about 10%. At a given spherical harmonic degree, the frequency spacing between peaks in the data generally decreases with increasing frequency, because the lower turning point of the waves is moving inward. However, between 5 and 5.5 mHz the frequency spacing increases slightly. This feature is probably associated with the acoustic cutoff frequency in the solar atmosphere, i.e., it indicates a transition from trapped waves to propagating waves. We are able to reproduce the observed behavior by a crude modeling of the solar atmosphere. Further study of these peaks should provide an independent way of exploring the mean structure of the solar atmosphere, particularly around the temperature minimum region.

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