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Titlebook: Chromospheric Fine Structure; R. Grant Athay Book 1974 International Astronomical Union 1974 Chromosphere.Corona.LOPES.Sunspot.solar.sun

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Michele Averchi,Emanuele Colombon measure’. Theoretical predictions for . (.) on the basis of a simple, one dimensional, steadily expanding atmosphere are presented. Depending upon the boundary conditions, and essentially upon the mass flux, two very different behaviours show up..The suggestion is made that a single model can reco
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https://doi.org/10.1007/978-3-319-39787-0alues of certain properties of the elements of the chromospheric fine structure by comparing the observed profiles of strong Fraunhofer lines with a simple theoretical formula involving four free parameters. The method is only applicable if two basic conditions are met: (1) The absorption coefficien
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Michele Averchi,Emanuele ColomboThe line formations of H. and Ca. H and K are compared in order to differentiate the various mechanisms giving rise to observable contrasts in the emergent intensities. Table II summarizes the criteria for distinguishing between horizontal spatial variations in temperature, density, and turbulent velocity.
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Comparison of H, and Ca, H and K Spectro-heliograms as a Diagnostic ProbeThe line formations of H. and Ca. H and K are compared in order to differentiate the various mechanisms giving rise to observable contrasts in the emergent intensities. Table II summarizes the criteria for distinguishing between horizontal spatial variations in temperature, density, and turbulent velocity.
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International Astronomical Union Symposiahttp://image.papertrans.cn/c/image/226364.jpg
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Chromospheric Fine Structure978-94-010-2103-6Series ISSN 1743-9213 Series E-ISSN 2352-2186
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Zusammenfassung der Untersuchungsergebnisse,ge about spicules both from limb and disk observations, also because it does not seem feasible to discuss the problem of . between spicules and their surroundings without starting by what is known about spicules themselves.
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