Jan 1983
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983soph...82..139r&link_type=abstract
(International Astronomical Union and Akademiia Nauk SSSR, Colloquium on Problems of Solar and Stellar Oscillations, 66th, Nauch
Physics
20
Astrometry, Solar Diameter, Solar Limb, Solar Oscillations, Atmospheric Effects, Brightness, Fourier Transformation, Oblate Spheroids, Power Spectra, Secular Variations
Scientific paper
Two definitions are possible for the solar diameter: astrophysical, relating to a specific physical parameter, or observational, relating to a given quantity that is to be measured. Since only the latter is directly accessible, astrophysical definitions should be linked to these quantities. All current solar diameter programs refer to the point of the limb where the brightness gradient is maximum, or to a higher order approximation of the profile shape. Two such programs, the Pic-du-Midi experiment which uses fast scans of the limb to define the injection point after a correction for atmospheric blurring, and the SCLERA experiment, employing an algorithm to obviate this correction, are compared. The advantage of a fast scan is noted.
Rösch Jean
Yerle Raymond
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