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Profile variations

In their paper, DLS claim that they observed, on one spectrum, a small emission around phase $\varphi \sim 0.78$ in the violet wing of the CaiiK line in only one of the two consecutive pulsation cycles they monitored.


  
Figure: The thin line is the average spectrum corresponding to Fig.1. The thick lines represent the spectra of $\rho$Pup around pulsation phases (indicated on the right of the figure) $\varphi = 0.78$ and 1.78. The width and the height of the emission detected by DLS is represented by the small inverse ``T'' symbol at our two expected emission phases $\varphi = 0.78$ and 1.78. The small shifts between the different spectra and the average one are mainly due to normalization process. Note that the scale is the same as the one used by DLS
\begin{figure}
\resizebox {\hsize}{!}{\includegraphics{fig3.ps}}\end{figure}

Fig.[*] shows that no particular emission, such as the one observed by DLS, is present. However, as mentionned in PaperI, the best way to detect the presence of the emission is to display the differential spectra, obtained by subtraction of each spectrum from a mean spectrum representing their average over one pulsation cycle. Results are presented in Fig.[*]. The changes between consecutive files are continuous and only reveal the atmospheric pulsation motion. Obviously, no emission feature is detected here.


  
Figure: All the differential spectra are represented, at the same scale as that of Fig.3. The continuous vertical line corresponds to the wavelength at which the emission occurs in DLS. The dashed vertical line corresponds to the laboratory wavelength. The small inverse ``T'' symbol has the same meaning as in Fig.3
\begin{figure}
\resizebox {\hsize}{!}{\includegraphics{fig4.ps}}\end{figure}


next up previous
Next: Discussion and conclusion Up: Results Previous: Radial velocities

8/13/1998