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Figure 1: The spectrum of HD 45677 during 1995-2001. The spectrograms, normalized to the continuum and vertically shifted, are, from top to bottom, of 14/01/1995 (R=7000), 19/10/1995 (R=36 000), 2/2/1999 (R=15 000) and 5/12/2001 (R=15 000). All the spectra were obtained at OHP with AURELIE, except the October 1995 one which is from the Russian Special Astrophysical Observatory. On the higher resolution spectrograms the deep Cr  II absorptions at 4558 and 4588 Å show up clearly.

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In the text

Figure 2: The two most intense lines of multiplet 44 of Cr  II observed the 5/12/2001, showing the central absorption well below the continuum and the three Gaussian components' fit. Each line profile (solid line) is fitted (dotted line) by three Gaussian components (dashed line). The residual (long dashed line) appears around the continuum (straight line). Notice the rising of the residual towards shorter wavelengths which is in both cases due to the presence of a strong Fe  II line.

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In the text

	Figure 4: Profiles and various components of the blend 4508.288 Å (Fe  II multiplet 38), 4509.610 Å ([Fe II] multiplet 6F) on the 2/2/1999 (see Fig. 2 for the explanation of the different curves). The different component FWHM are given in the text.
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In the text

	Figure 5: Profiles and various components of 5273.38 Å ([Fe II] multiplet 18F), 5276.002 Å (Fe  II multiplet 49), and 5278.374 Å ([Fe  II] multiplet 35F) on the 3/2/1999 (see Fig. 2 for the explanation of the different curves).The different component FWHM are given in the text.
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In the text

	Figure 6: Upper panel: Log normalized fluxes versus plots for the narrow components of Fe  II multiplets 27 (circle), 38 (square), 48 (triangle) with common upper term in the 1999 spectrum of HD 45677. Lower panel: log normalized fluxes versus plots of multiplets 27, 38 and 48. The multiplets are horizontally shifted according to the population ratio of their lower terms by p = 1.3.
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In the text

Figure 7: Global SAC of the narrow emission components in the 1999 spectrum of HD 45677. Results from the least squares overlapping of multiplets 27, 28, 32, 37, 38, 41, 42, 48, 49 and 74. The representative points are shifted horizontally and vertically according to a least squares fitting procedure by log level population corresponding to excitation temperatures of 3900 K and 3150 K for the lower and upper terms respectively.

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In the text

	Figure 8: SAC of broad components of multiplets 27, 28, 32, 37, 38, 41, 42, 48, 49 and 74 of Fe  II in 1999. The representative points are shifted horizontally and vertically by log level population corresponding to excitation temperatures of respectively 3900 K and 3400 K.
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In the text

	Figure 9: Position of the high excitation Fe  II lines (filled triangles) in the 1999 spectrum of HD 45677 with respect to the global SAC of Fig. 7. The multiplet 37 lines (filled squares) are shown for comparison.
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In the text

	Figure 10: SAC diagram of narrow components of multiplets 4F, 6F, 7F, 17F, 18F, 19F, 20F and 21F of [Fe  II] in 1999. The same mean level excitation temperature of 10 500 K has been used for both lower and upper levels. The observational points are interpolated with horizontal line.
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In the text

	Figure 11: SAC diagram of broad components of multiplets 4F, 6F, 7F, 17F, 18F, 19F, 20F and 21F of [Fe  II] in 1999. The representative points are shifted horizontally and vertically by log level population corresponding to an excitation temperature of 8500 K.
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In the text

	Figure 12: Self Absorption Curve for the narrow components of Cr  II emission lines.
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In the text

	Figure 13: Self Absorption Curve for the broad components of the Cr  II emission lines.
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In the text

Figure 14: Histogram of the emitting material radial velocities of an optically thin disk plus polar wind. The disk is inclined 85 to the sky plane with a total opening angle of 24. The velocity in the disk is 150  at the photospheric radius r=1, and the law is Keplerian. The polar wind is emitted in a 30 cone with a velocity of 100  at the pole and decreases exponentialy. In this figure and in Figs. 15 and 16, the synthetised profile and the continuum are plotted as a solid line, each Gaussian component as a short dashed line, the total fit profile as a dotted line and the residual flux as a long dashed line.

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In the text

Figure 15: Theoretical profile corresponding to the histogram of the emitting material radial velocities of an optically thin Keplerian disk inclined 12 on the sky plane. An accreting wind generates the broad component. The total fit profile coincides with the broad component for large velocities, and with the sum of the components for small velocities. The component FWHM are the ones derived in Sect. 2.2. The Keplerian velocity is equal to 340  at the photospheric radius r=1. The emission comes from 5<r<9, in photospheric radius unit.

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In the text

Figure 16: Theoretical profile corresponding to the histogram of the emitting material radial velocities of an optically thin Keplerian disk inclined 12 on the sky plane. An accreting wind generates the broad component. The component FWHM are the ones derived in Sect. 2.2. The Keplerian velocity is equal to 340  at the photospheric radius r=1. The emission comes from 15<r<20, in photospheric radius unit.

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In the text

Figure 17: Relative population of the levels in the [ ] (squares), and in the low and high excitation emission regions derived from the narrow emission components measured in the 1999 spectrum of HD 45677. The fluxes of the lower excitation emission lines (open circles) have been corrected for self-absorption, as discussed in the text. The high excitation emission lines are drawn as triangles. The straight lines represent the mean excitation temperatures of the upper levels of the [Fe  II] and of the lower and upper levels of the Fe  II emission lines, respectively. The crossing at 4.72 eV marks the connection between the lower (3900 K) and upper (3150 K) Fe  II level population laws. The zero points Y(0 eV) are the estimated ground level relative populations.

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In the text

	Figure 3: The Na ID lines in 1995 ( top), 1999 ( middle), 2002 ( bottom) and the fitted components. The profile (solid line) is fitted (dotted line) by two Gaussian components whose parameters (wavelength, flux, FWHM) are displayed in the right upper corner. The residual (long dashed line) appears around the continuum (straight line).
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In the text