Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{2054fg1a.ps}\end{figure}$ Figure 1: Lightcurves for AD Leo. From top: EPIC lightcurve, flare hardness ratio, time derivative of the X-ray lightcurve, and radio lightcurve at 5 GHz. The time axis is labelled in days after IAT midnight on 14.05.2001 (IAT differs from UT by the addition of 32 s). The identified X-ray flares are marked with dotted lines and labelled at the top of the plot.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{2054fg1b.ps}\hspace*{1cm} \includegraphics[width=7.8cm,clip]{2054fg1c.ps}\end{figure}$ Figure 2: Left: closeup of the radio lightcurve for the first radio event. The top panel shows the L flux, and the lower panel the R flux. The gap is the break between scans, during which time the phase calibrator was observed. Right: closeup of the event at 1.2 days (event C), showing the relative timing of the X-ray flux, derivative of X-ray flux and radio flux.
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In the text

$\begin{figure} \par\includegraphics[width=6.6cm,clip]{2054fg2a.ps}\vspace*{6mm} \par\includegraphics[width=6.6cm,clip]{2054fg2b.ps}\end{figure}$ Figure 3: Top: estimated kinetic energy of the emitting particles in the AD Leo flare at T=1.05 days (event A) as a function of $\delta$ and B. The solid contours show values of log(energy). Half decades are shown with dotted lines. The contour corresponding to the estimated radiated X-ray energy (approximately $7\times 10^{31}$ erg) is marked with a bold solid line. Bottom: the equivalent plot for event C.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{2054fg3a.ps}\vspace*{5mm} \par\hspace*{-3mm}\includegraphics[width=7.5cm,clip]{2054fg3b.ps}\end{figure}$ Figure 4: Upper figure, from top to bottom: X-ray flux, hardness ratio, derivative of X-ray flux and radio flux for AU Mic. The time axis is labelled in days since IAT midnight on 13.10.2000. Lower figure: close up of lightcurves around event C.
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In the text

$\begin{figure} \par\includegraphics[width=6.6cm,clip]{2054fg4a.ps}\hspace*{1.1cm} \includegraphics[width=6.6cm,clip]{2054fg4b.ps} \end{figure}$ Figure 5: Estimated kinetic energy of the emitting particles in the AU Mic radio flares corresponding to X-ray flares C ( on the left) and G ( on the right) as functions of $\delta$ and B. The solid contours show values of log(energy). Half decades are shown with dotted lines. The bold solid lines show the radiated X-ray energy. This was approximately $1.5\times 10^{32}$ erg for event C and $9\times 10^{31}$ erg for event G.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{2054fig5.ps}\end{figure}$ Figure 6: AT Mic lightcurves. From top to bottom, X-ray flux, hardness ratio, derivative of X-ray flux, and radio flux. The time axis is labelled in days since IAT midnight on 15.10.2000.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{2054fig6.ps}\end{figure}$ Figure 7: Lightcurves for UV Ceti. From the top, the X-ray flux, hardness ratio, derivative of the X-ray flux, 8.3 GHz flux and 5 GHz flux. The time is in IAT days after IAT = 0h on 07.07.2001.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{2054fg7a.ps}\vspace*{3mm} \par\includegraphics[width=8.2cm,clip]{2054fg7b.ps}\end{figure}$ Figure 8: Closeup of event A ( top) and event B ( bottom) for UV Cet.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{2054fig8.ps}\end{figure}$ Figure 9: Lightcurves for YZ CMi. The layout is the same as for previous cases for AD Leo, AU Mic and AT Mic. The time axis is labelled in days since 9.10.2000.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{2054fig9.ps}\end{figure}$ Figure 10: Cross correlation of the X-ray and radio lightcurves for the five targets. Correlations of $\pm$ 0.5 are indicated with dotted lines. The overall lightcurves do not correlate well, with the exception of AU Mic which has a peak correlation of 0.72.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{2054f10a.ps}\hspace*{7mm} \includegraphics[width=7.8cm,clip]{2054f10b.ps}\end{figure}$ Figure 11: Left: comparison of radiated X-ray energy with inferred particle energy for ten events in which plausible radio counterparts to X-ray flares could be identified. Each point is labelled with the first two letters of the stars' name and the identification letter of the flare in question. Right: the value of B for each of the ten events for which the particle kinetic energy matches the radiated X-ray energy for $\delta =3$ . This is the maximum value of B possible with that assumption. The straight line shows the relation $B \propto E_{\rm X}^{-0.4}$ , which is expected in the event that the radio flux is uncorrelated with the X-ray flux. The events AD A, AD C, AU C and AU G are shown in detail in the various contour plots above.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{2054fg1a.ps}\end{figure}$	Figure 1: Lightcurves for AD Leo. From top: EPIC lightcurve, flare hardness ratio, time derivative of the X-ray lightcurve, and radio lightcurve at 5 GHz. The time axis is labelled in days after IAT midnight on 14.05.2001 (IAT differs from UT by the addition of 32 s). The identified X-ray flares are marked with dotted lines and labelled at the top of the plot.
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$\begin{figure} \par\includegraphics[width=7.9cm,clip]{2054fg1b.ps}\hspace*{1cm} \includegraphics[width=7.8cm,clip]{2054fg1c.ps}\end{figure}$	Figure 2: Left: closeup of the radio lightcurve for the first radio event. The top panel shows the L flux, and the lower panel the R flux. The gap is the break between scans, during which time the phase calibrator was observed. Right: closeup of the event at 1.2 days (event C), showing the relative timing of the X-ray flux, derivative of X-ray flux and radio flux.
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$\begin{figure} \par\includegraphics[width=7.9cm,clip]{2054fg3a.ps}\vspace{5mm} \par\hspace{-3mm}\includegraphics[width=7.5cm,clip]{2054fg3b.ps}\end{figure}$	Figure 4: Upper figure, from top to bottom: X-ray flux, hardness ratio, derivative of X-ray flux and radio flux for AU Mic. The time axis is labelled in days since IAT midnight on 13.10.2000. Lower figure: close up of lightcurves around event C.
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$\begin{figure} \par\includegraphics[width=7.9cm,clip]{2054fig5.ps}\end{figure}$	Figure 6: AT Mic lightcurves. From top to bottom, X-ray flux, hardness ratio, derivative of X-ray flux, and radio flux. The time axis is labelled in days since IAT midnight on 15.10.2000.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{2054fig6.ps}\end{figure}$	Figure 7: Lightcurves for UV Ceti. From the top, the X-ray flux, hardness ratio, derivative of the X-ray flux, 8.3 GHz flux and 5 GHz flux. The time is in IAT days after IAT = 0h on 07.07.2001.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{2054fg7a.ps}\vspace*{3mm} \par\includegraphics[width=8.2cm,clip]{2054fg7b.ps}\end{figure}$	Figure 8: Closeup of event A ( top) and event B ( bottom) for UV Cet.
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$\begin{figure} \par\includegraphics[width=8.1cm,clip]{2054fig8.ps}\end{figure}$	Figure 9: Lightcurves for YZ CMi. The layout is the same as for previous cases for AD Leo, AU Mic and AT Mic. The time axis is labelled in days since 9.10.2000.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{2054fig9.ps}\end{figure}$	Figure 10: Cross correlation of the X-ray and radio lightcurves for the five targets. Correlations of $\pm$ 0.5 are indicated with dotted lines. The overall lightcurves do not correlate well, with the exception of AU Mic which has a peak correlation of 0.72.
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