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Figure 1: The analytic fit of HeII-impact broadening data for Sii 6142 Å line: a) Stark width, and b) Stark shift. The shift and width are given for one perturber per cm3. |
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Figure 2: A comparison between the observed Sii 6155 Å line profile in the solar spectrum and synthetic spectra calculated with Stark widths and shifts from Table 1 (solid line) and with Stark widths calculated by the approximate formulae and without Stark shift taken into account (dotted line). X- and Y-coordinates are wavelenghths and surface fluxes (normalized to unity). |
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Figure 3: The same as in Fig. 2 for normal star HD 32115. |
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Figure 4: The same as in Fig. 2 for Ap star HD 122970. |
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Figure 5: A comparison between the observed Sii 6155 Å line profile in the spectrum of Ap star 10 Aql (thick line) and synthetic spectra calculated with Stark widths and shifts from Table 1 and Si abundance stratification (thin line), with the same Stark parameters but for homogeneous Si distribution (dashed line), and with Stark width calculated by approximate formulae for the same stratification (dotted line). X- and Y-coordinates are wavelenghths and surface fluxes (normalized to unity). |
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Figure 6: The same as in Fig. 5 but for Sii 6142 Å line. |
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Figure 7: Si abundance distribution in the atmosphere of Ap star 10 Aql. |
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Figure 8:
A comparison between the observed Si II 6371 Å line profile
in the spectrum of Ap star 10 Aql (double line) and the synthetic spectrum calculated with
Si abundance distribution shown in Fig. 7 (solid line) and Si homogeneous
abundance
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