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• W2065749574 abstract "view Abstract Citations (4) References Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS A Theoretical Study of the Calcium II H and K Lines and Infrared Triplet in the Solar Chromosphere. Linsky, Jeffrey Abstract K Lines and Infrared Triplet in the Solar Chromosphere. JEFFREY LINsKY, Smithsonian Astrophysical Observatory and Department of Astronomy, Harvard University.-Statistical equilibrium equations have been formulated for a model calcium ii ion consisting of four discrete levels (32S, 32D, 42P~, 42P~) and a continuum. These equations have been solved iteratively, on the basis of the approach of Avrett and Loeser to yield non-LTE source functions for the H and K lines as well as for each of the lines in the infrared triplet (8498A, 8542A, and 8660A) under a range of physical conditions appropriate to the solar chromosphere. A computer program has been written to solve for these source functions and non-LTE ionization equilibria and to calculate emergent profiles on and off the disk as well as for heights and optical depths corresponding to features in these profiles. Comparison of a number of computed profiles with the data of Goldberg, Mohler, and Muller (Asfrophys. J. 129, 119, 1958) suggests the following preliminary conclusions: (1) The emission features H2 and K2 correspond to heights 600-900 km above the photosphere and optical depths 102 to 10~ in the center of the K line. (2) A natural consequence of chromospheric temperature distributions is that the K-line residual intensities are larger than those for the H line. (3) An upper limit of about 5 km/sec for the turbulent velocities in the region of formation of H2 and K2, 100O~3000 km is established by the visibility of the emission features corresponding to the relative maxima in the source functions. (4) Computed K-line profiles for the chromospheric models of Bohm-Vitense (Z. Astrophys. 36, 145, 1955) and Thomas and Athay (Physics of the Solar Chromosphere) and for the Utrecht reference model (Bull. Astron. Inst. Neth. 17, 442, 1964) yield K2 and K8 features that are between a factor of 5 and 10 larger than those observed. Unless the gas and electron densities are factors of 30 to 100 too high in these models for the low chromosphere, an electron temperature minimum of 4000 K and temperature less than 50000K at 1000 km are required. (5) When either the 32D level or the 42P+ level is ignored, the resultant source functions differ at most by a factor of 2, and the residual intensities by 1 % of the continuum from those computed, including all these levels. Publication: The Astronomical Journal Pub Date: February 1966 DOI: 10.1086/110047 Bibcode: 1966AJ.....71Q.391L full text sources ADS |" @default.
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• W2065749574 title "A Theoretical Study of the Calcium II H and K Lines and Infrared Triplet in the Solar Chromosphere." @default.
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