Abstract
The polarization distribution in the sky during a total solar eclipse is calculated with a simple secondary light-scattering model. This model uses the light-intensity measurements near the horizon during the eclipse and the pretotality and posttotality skylight polarization observations as input. It is found that the model can explain various observations during totality, including the quantitative measurements of Shaw [ Appl. Opt.14, 388 ( 1975)] of the polarization distribution of the sky in the solar vertical during the 1973 total eclipse.
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