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Solar scintillations were investigated as a method of detecting seeing-dependent wavefront curvature variations for solar adaptive optics. The method is applicable to full-disk averaged, adaptive corrections of large-scale near-field seeing distortions. As a test case, seeing measurements were carried out on a single small adaptive mirror, representing one element of what would be a large multielement adaptive array. All observations showed a greater than 5× reduction of seeing distortions as a result of this wavefront correction. 相似文献
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E. J. Seykora 《Solar physics》1993,145(2):389-397
A non-telescopic method of determining the quality of atmospheric seeing is discussed for large angular diameter objects, such as the Sun. In this method the concept of thermodynamic fluctuations is used to relate the observed intensity fluctuations to the r.m.s. angular diameter of the atmospheric seeing cells and telescopic angle of arrival fluctuations. Comparison between the measured r.m.s. cell size and telescopic angle of arrival fluctuations are presented for various degrees of seeing. Cross-correlation coefficients of 0.95 have been measured during such comparisons.Operated by the Association of Universities for Research in Astronomy, Inc. (AURA), under cooperative agreement with the National Science Foundation. Partial support for NSO is provided by USAF under a Memorandum of Understanding with the NSF. 相似文献
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E. J. Seykora 《Solar physics》1985,99(1-2):39-42
The spatial derivative of the intensity structure of the photosphere has been investigated utilizing a differential photometer system capable of recording intensity variations on the solar disc of 0.05% per arc sec. Time evolution images of the differential intensity profile for a 562.5 arc sec segment of the solar photosphere show a high degree of structure. To a large extent the observed structure persists for times greater than one hour and is rather highly ordered in spatial distribution. Power spectra of the spatial structure averaged over one hour show maxima at 28000 km and 16000 km, close to the spatial scale expected for intensity perturbations from supergranulation.Operated by the Association of Universities for Research in Astronomy, Inc. under contract with the National Science Foundation. 相似文献
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