Abstract
Calculations are made for the center-limb variations of the K2 and K3 components of the solar Ca ii K line using an optically thick model of the chromosphere. The center-limb variations are shown to require an increase of Doppler width with height in the chromosphere and to depend critically upon the location of the point where Δλ D has increased by a factor e. Good agreement with observations is found when, and only when, the increase in Δλ D occurs nearly simultaneously with the increase in chromospheric temperature.
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Athay, R.G., Skumanich, A. Emission cores in H and K lines. Sol Phys 4, 176–184 (1968). https://doi.org/10.1007/BF00148079
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DOI: https://doi.org/10.1007/BF00148079