Abstract
HD 87643 is one of the B[e] stars that still defy our understanding to better classify it. The spectroscopic observations of HD 87643 performed in the Astronomical Observatory of La Silla (ESO) between December 1998 and April 2000 show an object far more complex than was already known, with profiles of the Balmer series showing variability on different time scales. This work examine the formation of Hα and Hβ profiles with the SEI method (Sobolev approximation with Exact Integration of the transfer equation), as well as their spectral energy distribution by means of codes Cloudy and Dusty. For a homogeneous and spherically symmetric nebula around a star with T ef ~ 15, 000 K and log L/L⊙ > 4.2, the reproduction of the profiles mentioned was only achieved for Hβ and to some extent, considering two distinct regions with different laws for the expansion of the wind and with different rates of mass loss.
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