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FS CMa type stars are a recently described group of objects with the B[e]phenomenon that exhibit strong emission-line spectra and strong IR excesses. Inthis paper we report the first attempt for a detailed modeling of IRAS00470+6429, for which we have the best set of observations. Our modeling isbased on two key assumptions: the star has a main-sequence luminosity for itsspectral type (B2) and the circumstellar envelope is bimodal, composed of aslowly outflowing disk-like wind and a fast polar wind. Both outflows areassumed to be purely radial. We adopt a novel approach to describe the dustformation site in the wind that employs timescale arguments for graincondensation and a self-consistent solution for the dust destruction surface.With the above assumptions we were able to reproduce satisfactorily manyobservational properties of IRAS 00470+6429, including the H line profiles andthe overall shape of the spectral energy distribution. Our adopted recipe fordust formation proved successful in reproducing the correct amount of dustformed in the circumstellar envelope. Possible shortcomings of our model, aswell as suggestions for future improvements, are discussed.

Towards Understanding The B[e] Phenomenon: IV. Modeling of IRAS 00470+6429