Astronomy & Astrophysics

All Figures

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[clip]{h4599_f01.eps}} \end{figure}$ Figure 1: Observing Journal for our monitoring of V410 Tau in Nov. 2001. Note, that our campaign includes a third Chandra observation which was performed in March 2002 and is not shown in this diagram.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{h4599_f02.eps} \end{figure}$ Figure 2: O-C diagram for the seasonally averaged times of minimum T₀ in the V band lightcurve of V410 Tau versus rotational cycle number N. Open circles - for the period given by P94, and filled circles - after adapting the period to minimize the residuals. Data obtained in Nov. 2001 were used as reference point.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{h4599_f03a.eps} \end{figure}$ Figure 3: Seasonally averaged V band lightcurves of V410 Tau from 1981 to 2001 phase folded with the new ephemeris given in Table 2 (continued on the next page). Data are extracted from the data base maintained by W. Herbst. The data for 2001 was obtained by one of us (KG) in the months prior to our coordinated observing campaign.
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In the text

$\begin{figure}\par\includegraphics[width=8.5cm,clip]{h4599_f03b.eps}\hspace*{4mm} \includegraphics[width=8.5cm,clip]{h4599_f03c.eps} \end{figure}$ Figure 3: continued.
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In the text

$\begin{figure} \par\includegraphics[width=15.5cm,clip]{h4599_f04.eps} \end{figure}$ Figure 4: Longterm behavior of amplitude, mean, and maximum and minimum of the V band lightcurve of V410 Tau from 1978 to 2001. Data points represent seasonal averages. The numbers on the top y-axis stand for the year in which the observing season started.
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In the text

$\begin{figure} \par\includegraphics[width=18cm,clip]{h4599_f05.eps} \end{figure}$ Figure 5: Multi-wavelength phase plot for the 1.87 d cycle of V410 Tau. From top to bottom: Radial velocity, equivalent width of H $\alpha$ , X-ray count rate, and V band photometry. Except for some data points in the radial velocity curve all measurements are obtained quasi-simultaneously in November 2001. The large flare visible in the V band lightcurve was also observed spectroscopically, but the equivalent widths of H $\alpha$ are outside the range displayed in this figure (see Fernández et al., in prep. for a detailed discussion). The fast increase of the X-ray count rate near $\phi = 0$ (marked with an arrow) probably indicates the beginning of a flare (see Sect. 5).
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[clip]{h4599_f06.eps}} \end{figure}$ Figure 6: Quiescent X-ray spectrum of V410 Tau during three Chandra exposures. A flare has been eliminated from Obs. Seq.# 200130. The data are overlaid by the best fit model from Table 3. The residuals for each observation are shown in separate panels.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[clip]{h4599_f07.eps}} \end{figure}$ Figure 7: ACIS hardness ratios for V410 Tau. Flare and quiescent state for observation 200130 are labeled with "F'' and "Q'', respectively. Error bars denote 1 $\sigma$ uncertainties.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[clip]{h4599_f01.eps}} \end{figure}$	Figure 1: Observing Journal for our monitoring of V410 Tau in Nov. 2001. Note, that our campaign includes a third Chandra observation which was performed in March 2002 and is not shown in this diagram.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{h4599_f02.eps} \end{figure}$	Figure 2: O-C diagram for the seasonally averaged times of minimum T₀ in the V band lightcurve of V410 Tau versus rotational cycle number N. Open circles - for the period given by P94, and filled circles - after adapting the period to minimize the residuals. Data obtained in Nov. 2001 were used as reference point.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{h4599_f03a.eps} \end{figure}$	Figure 3: Seasonally averaged V band lightcurves of V410 Tau from 1981 to 2001 phase folded with the new ephemeris given in Table 2 (continued on the next page). Data are extracted from the data base maintained by W. Herbst. The data for 2001 was obtained by one of us (KG) in the months prior to our coordinated observing campaign.
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$\begin{figure}\par\includegraphics[width=8.5cm,clip]{h4599_f03b.eps}\hspace*{4mm} \includegraphics[width=8.5cm,clip]{h4599_f03c.eps} \end{figure}$	Figure 3: continued.
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$\begin{figure} \par\includegraphics[width=15.5cm,clip]{h4599_f04.eps} \end{figure}$	Figure 4: Longterm behavior of amplitude, mean, and maximum and minimum of the V band lightcurve of V410 Tau from 1978 to 2001. Data points represent seasonal averages. The numbers on the top y-axis stand for the year in which the observing season started.
Open with DEXTER

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[clip]{h4599_f06.eps}} \end{figure}$	Figure 6: Quiescent X-ray spectrum of V410 Tau during three Chandra exposures. A flare has been eliminated from Obs. Seq.# 200130. The data are overlaid by the best fit model from Table 3. The residuals for each observation are shown in separate panels.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[clip]{h4599_f07.eps}} \end{figure}$	Figure 7: ACIS hardness ratios for V410 Tau. Flare and quiescent state for observation 200130 are labeled with "F'' and "Q'', respectively. Error bars denote 1 $\sigma$ uncertainties.
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