All Figures

$\begin{figure} \par\includegraphics[width=16.8cm,clip]{6536_f1.eps}\end{figure}$ Figure 1: Light curves and spectral fitting results for the flaring TMC sources V410 X7 (XEST-23-050/24-042) and V819 Tau (XEST-23-074/24-061). In the top panels, the background-subtracted PN light curve of each source is plotted with a thick solid line, while the thin solid line shows the background light curve, scaled to the source area. The vertical dotted lines mark the time intervals, derived from the MLB analysis, used for the time-resolved spectroscopy. In the other panels we show, from top to bottom, the time evolution of the best-fit temperatures, emission measures, and hydrogen column density. The temperatures and EMs of the cool and hot components are indicated by diamonds and asterisks, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=16.7cm,clip]{6536_f2.eps}\end{figure}$ Figure 2: Left: light curve and spectral fitting results for HBC 427 (XEST-26-072). Panels are the same as in Fig. 1. Note that in this case we show the combined MOS1+MOS2 light curve, the PN being not available. Right: evolution of the best-fit temperature and EM of the hot component for HBC 427. To better clarify the trend with time of the parameters, the points are connected by dotted lines. The thick solid line shows the linear fitting to points #3 to #7, corresponding to the flare decay; for clarity they are marked with open squares.
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In the text

$\begin{figure} \par\includegraphics[width=16.4cm,clip]{6536_f3.eps}\end{figure}$ Figure 3: Left: light curve and spectral fitting results for BP Tau (XEST-28-100). Panels are the same as in Fig. 1. Right: evolution of the best-fit temperature and EM of the hot component. See Fig. 2 for details. For the sake of clarity, we plot only the points from #2 to #9. The slope has been fitted between points #4 and #8.
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In the text

$\begin{figure} \par\includegraphics[width=16.8cm,clip]{6536_f4.eps}\end{figure}$ Figure 4: Light curve and spectral fitting results for the TMC sources JH 108 (XEST-17-066) and V892 Tau (XEST-23-047/24-040) showing gradual rise flares. Panels are the same as in Fig. 1.
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In the text

$\begin{figure} \par\includegraphics[width=16.85cm,clip]{6536_f5.eps}\end{figure}$ Figure 5: Left: light curve and spectral fitting results for V410 Tau (XEST-23-032/24-028). Panels are the same as in Fig. 1. Right: evolution of the best-fit temperature and EM of the hot component. See Fig. 2 for details. For the sake of clarity, we plot only the points from #7 to #15. The slope has been fitted between points #8 and #14.
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In the text

$\begin{figure} \par\includegraphics[width=16.8cm,clip]{6536_f6.eps}\end{figure}$ Figure 6: Light curve and spectral fitting results for TMC sources showing a long-lasting rise (XZ Tau = XEST-22-047) or decay (V830 Tau = XEST-04-016, HQ Tau = XEST-09-026, FS Tau = XEST-11-057). Panels are the same as in Fig. 1.
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In the text

$\begin{figure} \par\includegraphics[width=16.8cm,clip]{6536_f7.eps}\end{figure}$ Figure 7: Same as Fig. 6 for DH Tau (XEST-15-040) and L1551 51 (XEST-22-089).
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In the text

$\begin{figure} \par\includegraphics[width=16.8cm,clip]{6536_f8.eps}\end{figure}$ Figure 8: Light curve and spectral fitting results for the TMC sources DN Tau (XEST-12-040) and HD 283572 (XEST-21-039), showing a slow modulation. Panels are the same as in Fig. 1.
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In the text

$\begin{figure} \par\includegraphics[width=8.15cm,clip]{6536_f9.eps}\end{figure}$ Figure 9: Light curve and spectral fitting results for the TMC source Hubble 4 (XEST-23-056/24-047) showing a complex variability. Panels are the same as in Fig. 1.
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In the text

$\begin{figure} \par\includegraphics[width=16.9cm,clip]{6536_f10.eps}\end{figure}$ Figure 10: Light curve and spectral fitting results for the XEST sources HD 283810 (XEST-05-031) and HD 285845 (XEST-22-024), not associated with the TMC. Panels are the same as in Fig. 1.
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In the text

$\begin{figure} \par\includegraphics[width=16.8cm,clip]{6536_f11.eps}\end{figure}$ Figure 11: Left: light curve and spectral fitting results for XEST-16-031. Panels are the same as in Fig. 1. Right: evolution of the best-fit temperature and EM of the hot component. See Fig. 2 for details. The slope has been fitted between points #10 and #14. The slope during the decay of the first small flare (points #4 and #5) is also indicated.
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In the text

$\begin{figure} \par\includegraphics[width=16.4cm,clip]{6536_f3.eps}\end{figure}$	Figure 3: Left: light curve and spectral fitting results for BP Tau (XEST-28-100). Panels are the same as in Fig. 1. Right: evolution of the best-fit temperature and EM of the hot component. See Fig. 2 for details. For the sake of clarity, we plot only the points from #2 to #9. The slope has been fitted between points #4 and #8.
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$\begin{figure} \par\includegraphics[width=16.8cm,clip]{6536_f4.eps}\end{figure}$	Figure 4: Light curve and spectral fitting results for the TMC sources JH 108 (XEST-17-066) and V892 Tau (XEST-23-047/24-040) showing gradual rise flares. Panels are the same as in Fig. 1.
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$\begin{figure} \par\includegraphics[width=16.85cm,clip]{6536_f5.eps}\end{figure}$	Figure 5: Left: light curve and spectral fitting results for V410 Tau (XEST-23-032/24-028). Panels are the same as in Fig. 1. Right: evolution of the best-fit temperature and EM of the hot component. See Fig. 2 for details. For the sake of clarity, we plot only the points from #7 to #15. The slope has been fitted between points #8 and #14.
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$\begin{figure} \par\includegraphics[width=16.8cm,clip]{6536_f6.eps}\end{figure}$	Figure 6: Light curve and spectral fitting results for TMC sources showing a long-lasting rise (XZ Tau = XEST-22-047) or decay (V830 Tau = XEST-04-016, HQ Tau = XEST-09-026, FS Tau = XEST-11-057). Panels are the same as in Fig. 1.
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$\begin{figure} \par\includegraphics[width=16.8cm,clip]{6536_f7.eps}\end{figure}$	Figure 7: Same as Fig. 6 for DH Tau (XEST-15-040) and L1551 51 (XEST-22-089).
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$\begin{figure} \par\includegraphics[width=16.8cm,clip]{6536_f8.eps}\end{figure}$	Figure 8: Light curve and spectral fitting results for the TMC sources DN Tau (XEST-12-040) and HD 283572 (XEST-21-039), showing a slow modulation. Panels are the same as in Fig. 1.
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$\begin{figure} \par\includegraphics[width=8.15cm,clip]{6536_f9.eps}\end{figure}$	Figure 9: Light curve and spectral fitting results for the TMC source Hubble 4 (XEST-23-056/24-047) showing a complex variability. Panels are the same as in Fig. 1.
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$\begin{figure} \par\includegraphics[width=16.9cm,clip]{6536_f10.eps}\end{figure}$	Figure 10: Light curve and spectral fitting results for the XEST sources HD 283810 (XEST-05-031) and HD 285845 (XEST-22-024), not associated with the TMC. Panels are the same as in Fig. 1.
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$\begin{figure} \par\includegraphics[width=16.8cm,clip]{6536_f11.eps}\end{figure}$	Figure 11: Left: light curve and spectral fitting results for XEST-16-031. Panels are the same as in Fig. 1. Right: evolution of the best-fit temperature and EM of the hot component. See Fig. 2 for details. The slope has been fitted between points #10 and #14. The slope during the decay of the first small flare (points #4 and #5) is also indicated.
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