Abstract
The central star V4334 Sgr (Sakurai's Nova) of the planetary nebula PN G010.4+04.4 underwent in 1995–1996 the rare event of a very late helium flash shell burning. The rapid formation of a dust shell allows a precise model, basing on the dust formation history instead of the commonly used average dust formation rate and mass loss. The model applies a complete dust grain size distribution, and transiently heated grains. Only the fitting of the visual light curve gives already the complete spectral energy distribution (SED) model. No adjustment with the infrared data points is needed.
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