All Figures

$\begin{figure} { \psfig{figure=2834fig1.ps,width=7.8cm} } \end{figure}$ Figure 1: The AT Mic 0.2-12 keV X-ray 10-s bin light curve (shown in black). Overplotted in white is the same light curve smoothed with a sliding time window of 200 s. The time is in ks, starting from the beginning of the observation (2000-10-16 00:42:00). The vertical dotted lines mark the flare start, end of rise phase, end of extended top phase and end of the flare.
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In the text

$\begin{figure} { \psfig{figure=2834fig2.ps,width=7.5cm} } \end{figure}$ Figure 2: The upper panel shows the 10-s bin light curve. The lower panel displays the high-frequency wavelet coefficients of the continuous wavelet transform of the above light curve, using a Morlet wavelet (see Sect. 3.2). The contours give the 68%, 95% and 99.9% significance levels. The dashed lines represent the cone of influence. The vertical dotted lines are the same as in Fig. 1. The arrow points to the flare oscillation in the wavelet domain and the horizontal dotted lines mark the division between the high (noise), medium (oscillation) and low frequency ranges.
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In the text

$\begin{figure} { \psfig{figure=2834fig3.ps,width=7.8cm} } \end{figure}$ Figure 3: The reconstructed light curve divided into three frequency bands, low ( $P>1200~{\rm s}$ ), medium (500 s < P < 1200 s, including the oscillation) and high (10 s < P < 500 s, mainly noise); together they add up to the original data (lowest panel). The shaded areas show the standard errors. The vertical dotted lines are the same as in Fig. 1. A coherent oscillation is easily identified during flare peak.
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In the text

$\begin{figure} { \psfig{figure=2834fig4.ps,width=7.8cm} } \end{figure}$ Figure 4: The flare part of the $P=500...1200~{\rm s}$ reconstructed light curve (Fig. 3, second panel). The vertical dotted lines bound the flare top. The solid line shows the reconstructed light curve from the data, whereas the dashed line is a damped sine curve (bounded by the exponential envelope, dashed-dotted line) with an oscillation period of P = 750 s and an exponential decay time of $\tau$ = 2000 s. The relative peak-to-peak amplitude is initially 15%.
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In the text

$\begin{figure} { \psfig{figure=2834fig1.ps,width=7.8cm} } \end{figure}$	Figure 1: The AT Mic 0.2-12 keV X-ray 10-s bin light curve (shown in black). Overplotted in white is the same light curve smoothed with a sliding time window of 200 s. The time is in ks, starting from the beginning of the observation (2000-10-16 00:42:00). The vertical dotted lines mark the flare start, end of rise phase, end of extended top phase and end of the flare.
Open with DEXTER