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A solar eclipse is a rare but spectacular natural phenomenon and  furthermore it is a challenge for radiative transfer modelling.  Whereas a simple one-dimensional radiative transfer model with  reduced solar irradiance at the top of the atmosphere can be used to  calculate the brightness during partial eclipses a much more  sophisticated model is required to calculate the brightness  (i.e. the diffuse radiation) during the total eclipse. The reason is  that radiation reaching a detector in the shadow gets there  exclusively by horizontal transport of photons in a spherical shell  atmosphere, which requires a three-dimensional radiative transfer  model. In this study the first fully three-dimensional simulations  for a solar eclipse are presented exemplified by the solar eclipse  at 29 March 2006. Using a backward Monte Carlo model we calculated  the diffuse radiation in the umbra and simulated the changing  colours of the sky. Radiance and irradiance are decreased by 3 to 4  orders of magnitude, depending on wavelength.  We found that aerosol  has a comparatively small impact on the radiation in the umbra. We  also estimated the contribution of the solar corona to the radiation  under the umbra and found that it is negligible compared to the  diffuse solar radiation in the wavelength region from 310 to 500 nm

Simulation of solar radiation during a total eclipse: a challenge for radiative transfer