Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3066f1.ps} \end{figure}$ Figure 1: Comparison between data collected during the same night (November 29, HJD = 2 452 243) at BAO (crosses), SAAO (open circles), and at JKT (filled circles).
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In the text

$\begin{figure} \par\includegraphics[width=15.7cm,clip]{3066f2.ps} \end{figure}$ Figure 2: Light curve of V351 Ori (points). The meaning of $\delta$ V (in magnitudes) is Variable-Comparison star. The winter 2001 and winter 2002 campaigns include data from HJD = 2 452 201 to HJD = 2 452 318 and from HJD = 2 452 567 to HJD = 2 452 586, respectively. The solid line shows the fit to the data obtained as described in Sect. 3.
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In the text

$\begin{figure} \par\includegraphics[width=15.7cm,clip]{3066f3.ps} \end{figure}$ Figure 3: Light curve of V351 Ori. Same as in Fig. 2.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{3066f4.ps} \end{figure}$ Figure 4: Spectral window for the 2001 dataset (upper panel), 2002 dataset (middle panel), and the whole dataset (lower panel). Note that the y-axis is in amplitude units.
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In the text

$\begin{figure} \par\includegraphics[width=15.7cm,clip]{3066f5.ps} \end{figure}$ Figure 5: Frequency analysis for the whole data set. Each panel shows the Fourier Transform after the subtraction of a pulsating frequency. The solid line corresponds to S/N=4. The dotted and dashed lines show the 99% and 90% significance level calculated from the Scargle (1982) test.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3066f6.ps} \end{figure}$ Figure 6: Phase diagrams for the five frequencies listed in Table 4. From top to bottom the data has been phased using frequencies f₁ to f₅).
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{3066f7.ps} \end{figure}$ Figure 7: Location in the HR diagram of the best fit models for V351 Ori (filled circle). The box (dashed lines and open triangles) indicates the range of luminosity and effective temperature corresponding to the empirical estimates available in the literature. Also shown are the evolutionary tracks by Palla & Stahler (1993) (solid lines), and the instability strip by Marconi & Palla (1998) (shaded area).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3066f1.ps} \end{figure}$	Figure 1: Comparison between data collected during the same night (November 29, HJD = 2 452 243) at BAO (crosses), SAAO (open circles), and at JKT (filled circles).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=15.7cm,clip]{3066f2.ps} \end{figure}$	Figure 2: Light curve of V351 Ori (points). The meaning of $\delta$ V (in magnitudes) is Variable-Comparison star. The winter 2001 and winter 2002 campaigns include data from HJD = 2 452 201 to HJD = 2 452 318 and from HJD = 2 452 567 to HJD = 2 452 586, respectively. The solid line shows the fit to the data obtained as described in Sect. 3.
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$\begin{figure} \par\includegraphics[width=15.7cm,clip]{3066f3.ps} \end{figure}$	Figure 3: Light curve of V351 Ori. Same as in Fig. 2.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{3066f4.ps} \end{figure}$	Figure 4: Spectral window for the 2001 dataset (upper panel), 2002 dataset (middle panel), and the whole dataset (lower panel). Note that the y-axis is in amplitude units.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=15.7cm,clip]{3066f5.ps} \end{figure}$	Figure 5: Frequency analysis for the whole data set. Each panel shows the Fourier Transform after the subtraction of a pulsating frequency. The solid line corresponds to S/N=4. The dotted and dashed lines show the 99% and 90% significance level calculated from the Scargle (1982) test.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3066f6.ps} \end{figure}$	Figure 6: Phase diagrams for the five frequencies listed in Table 4. From top to bottom the data has been phased using frequencies f₁ to f₅).
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