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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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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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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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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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Figure 6:
Upper panel: Log normalized fluxes versus
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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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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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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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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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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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Figure 12: Self Absorption Curve for the narrow components of Cr II emission lines. |
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Figure 13: Self Absorption Curve for the broad components of the Cr II emission lines. |
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Figure 14:
Histogram of the emitting material radial velocities of an optically
thin disk plus polar wind. The disk is inclined 85![]() ![]() ![]() ![]() ![]() |
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Figure 15:
Theoretical profile corresponding to the histogram of the emitting
material radial velocities of an optically thin Keplerian disk inclined
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Figure 16:
Theoretical profile corresponding to the histogram of the emitting
material radial velocities of an optically thin Keplerian disk inclined
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Figure 17:
Relative population of the
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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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