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We studied the circumstellar environment of the B[e] star HD 45677 throughthe analysis of the emission lines from ionized metals. We used the statisticalapproach of the self absorption curve method (SAC) to derive physicalparameters of the line emitting region. The Fe II and Cr II double-peakedemission line structure is explained by the presence of a thin absorptioncomponent red shifted by ~3 km/s. This absorption component can be interpretedgeometricaly as being due to infalling material perpendicularly to the diskseen nearly pole-on, as indicated by the emission line structure. The Cr II andFe II emission lines have a complex structure with two (narrow and broad)components, of 45 and 180 km/s FWHM for the permitted lines and 25 and 100 km/sFWHM for the forbidden ones, respectively. We argue that the narrow componentsare principaly emitted by an optically thin disk seen nearly pole-on, in aregion whose minimum radius is estimated to be 4 10^12 cm, while the broad onesare formed in a disk-linked wind.Comment: 14 pages, submitted to Astronomy and Astrophysic

Analysis of the circumstellar environment of the B[ e] star HD 45677 (FS Canis Majoris)