All Figures

$\begin{figure} \par\resizebox{18cm}{!}{\rotatebox{90}{\includegraphics{7657fg1a.eps}}}\end{figure}$ Figure 1: Light curves of V2104 Cyg obtained at SNO and SPMO in October-November 2005. The u (dots), v (stars), b (crosses) and y (+) magnitude differences are plotted in time (HJD-2453000). Note the difference in scale between the u and vby data: tickmarks in the u filter and vby filters correspond to 0.04 mag and 0.03 mag respectively. The light curves of all 15 nights are only available in the on-line version of the paper.
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In the text

$\begin{figure} \par\resizebox{17cm}{!}{\rotatebox{-90}{\includegraphics{7657fig2.eps}}} \end{figure}$ Figure 2: Left panel: Window function ( top) and SCARGLE periodograms of V2104 Cyg at different stages of the frequency search in the Strömgren v filter. The amplitudes are expressed in mmag. The detected frequencies $\nu _1$ $=4.7126\pm 0.0004$ d^-1 , $.\!\!^{\rm d}$ $=2.2342\pm 0.0005$ d^-1 and $\nu _3$ $=4.671\pm 0.001$ d^-1 are indicated by dashed vertical lines. The last but one bottom periodogram shows the final residuals after prewhitening with $\nu _1$ , $.\!\!^{\rm d}$ and $\nu _3$ . The light grey horizontal lines represent the (S/N>3.6)-level. In the bottom periodogram we present the variability of the comparison stars, illustrating that they are constant at the level of a few 0.1 mmag. Right panel: Phase diagrams of the 3 detected frequencies in the v filter. Black stars correspond to observations and the grey full lines represent the least-squares fit. The amplitudes are expressed in mag.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\rotatebox{-90}{\includegraphics{7657fig... ...resizebox{8.8cm}{!}{\rotatebox{-90}{\includegraphics{7657fig4.eps}}}\end{figure}$ Figure 3: The H $\alpha$ and H $\beta$ profiles of V2104 Cyg clearly show emission. The black profiles are FIES profiles while the grey H $\alpha$ profile is taken with the Elodie spectrograph. Between June 2006 and November 2006 the emission peak shifted and changed slightly in shape, indications for the dynamical character of the circumstellar disk.
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In the text

$\begin{figure} \resizebox{8.8cm}{!}{\rotatebox{-90}{\includegraphics{7657fig5.eps}}}\end{figure}$ Figure 4: Possible position of V2104 Cyg in the Hertzsprung-Russell diagram. The black square indicates the position derived from the observed photometric indices while the star indicates the position after correction for the contribution of the stellar disk. The full black lines and the dashed black lines represent the instability strips for the SPB and $\beta$ Cephei modes respectively, with a frequency between 0.25 and 25 d^-1 and $\ell \leq 4$ computed for Main Sequence models (De Cat et al. 2007). The dark grey dotted lines show the ZAMS and the TAMS.
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In the text

Full version

$\begin{figure} \par\resizebox{18cm}{!}{\rotatebox{90}{\includegraphics{7657fg1b.eps}}}\end{figure}$ Figure 1: Light curves of V2104 Cyg obtained at SNO and SPMO in October-November 2005. The u (dots), v (stars), b (crosses) and y (+) magnitude differences are plotted in time (HJD-2453000). Note the difference in scale between the u and vby data: tickmarks in the u filter and vby filters correspond to 0.04 mag and 0.03 mag respectively.
Open with DEXTER

In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\rotatebox{-90}{\includegraphics{7657fig... ...resizebox{8.8cm}{!}{\rotatebox{-90}{\includegraphics{7657fig4.eps}}}\end{figure}$	Figure 3: The H $\alpha$ and H $\beta$ profiles of V2104 Cyg clearly show emission. The black profiles are FIES profiles while the grey H $\alpha$ profile is taken with the Elodie spectrograph. Between June 2006 and November 2006 the emission peak shifted and changed slightly in shape, indications for the dynamical character of the circumstellar disk.
Open with DEXTER

$\begin{figure} \par\resizebox{18cm}{!}{\rotatebox{90}{\includegraphics{7657fg1b.eps}}}\end{figure}$	Figure 1: Light curves of V2104 Cyg obtained at SNO and SPMO in October-November 2005. The u (dots), v (stars), b (crosses) and y (+) magnitude differences are plotted in time (HJD-2453000). Note the difference in scale between the u and vby data: tickmarks in the u filter and vby filters correspond to 0.04 mag and 0.03 mag respectively.
Open with DEXTER