All Figures

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{4539fig1.ps} \end{figure}$ Figure 1: Comparing spot longitudes from our time series modelling (small crosses and dots with error bars) with results from Korhonen et al. (2002, 2004; big empty triangles and circles), and with spot longitudes measured in all Doppler images of FK Com available to us to date (Korhonen et al. 2005, bigger dots). The bi-modal distribution of spot longitudes is evident using all of the three different techniques. The longitudes are plotted betwen 0 $^\circ$ -360 $^\circ$ (marked with horizontal lines), with a very few exceptions, in most cases when the time series results moved continuously around 0 $^\circ$ .
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{4539fig2.ps}\end{figure}$ Figure 2: From top to bottom: FK Com data; spot radii (crosses: spot 1, dots: spot 2, triangles: polar spot); spot longitudes (crosses: spot 1, dots: spot 2) for the years 1987-2004. Broken vertical lines represent the times when the two low-latitude spots are 180 $^\circ$ apart from each other and continue moving closer on one or on the other side of the star, i.e. the flip-flop times. The shaded and clear time intervals in the bottom panel mark when the spots are closer to each other around 0 $^\circ$ and 180 $^\circ$ longitudes, respectively, i.e., in the two hemispheres of the star.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{4539fig3.ps} \end{figure}$ Figure 3: Top: the distribution of longitudes of the two low-latitude spots of FK Com when they are closer to each other a) around 0 $^\circ$ and b) around 180 $^\circ$ longitudes. Bottom: phased original observational data (with long-term, overall variability removed) from the time-intervals when spots are around 0 $^\circ$ (dots) and 180 $^\circ$ (crosses). See the bottom panel of Fig. 2 for further orientation.
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In the text

$\begin{figure} \par\includegraphics[width=3.7cm,clip]{4539fig4.ps}\end{figure}$ Figure 4: The distribution of longitude distances of the two low-latitude spots from the present results (horizontally shaded), from Korhonen et al. (2002, 2004; vertically shaded), and from Doppler maps (filled). Results of the present paper are plotted with respect to the left y-axis, the other results (lower in number) with respect to the right y-axis.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{4539fig5.ps} \end{figure}$ Figure 5: Time-series fit for the 1999 dataset. Note the continuous change in the amplitude and the practically vanished amplitude at JD 2 451 310; and, that the rotation period of FK Com is 2.4 days.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{4539fig6.ps}\end{figure}$ Figure 6: Time-series fit for the 1999 dataset ( top panel). The spot longitudes are shown in the middle panel (circles: spot 1, triangles: spot 2). Filled symbols are results taken from Korhonen et al. (2002). The bottom panel shows spot sizes (circles: spot 1, triangles: spot 2, squares: polar spot). Note the longitude discontinuity of spot 2 by about 90 $^\circ$ , and the disappearance of both spot 1 and spot 2 shortly after JD 2 451 300.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{4539fig7.ps} \end{figure}$ Figure 7: Modelling the 1999 dataset in 10 segments with light-curve inversion. Left panels show the data with the fits, the corresponding right panels are the maps of the spot filling factor. Note the very small amplitude in the light curve for this time period.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4539fig8.ps} \end{figure}$ Figure 8: Time-series fit for the 1997 dataset. The light variability changes smoothly and is never below 0.1 mag. A sudden change in the light curve shape is seen shortly after JD 2 450 500.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{4539fig9.ps} \end{figure}$ Figure 9: Time-series fit for the 1997 dataset ( top panel). The spot longitudes are shown in the middle panel (circles: spot 1, triangles: spot 2). Filled triangles are results of the light-curve inversion. The bottom panel shows spot sizes (circles: spot 1, triangles: spot 2, squares: polar spot). Note that spot 2 either disappeared or merged with spot 1 near JD 2 450 500, and a new spot 2 appeared shifted by about 100 $^\circ$ . The phase-jump is clearly seen from the light-curve inversion as well. The activity remained on the same hemisphere of the star.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{4539fi10.ps} \end{figure}$ Figure 10: Modelling the 1997 dataset in 10 segments with the light-curve inversion method. Left panels show the data with the fits, the corresponding right panels are the maps of the spot filling factor.
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In the text

$\begin{figure} \par\includegraphics[width=3.7cm,clip]{4539fig4.ps}\end{figure}$	Figure 4: The distribution of longitude distances of the two low-latitude spots from the present results (horizontally shaded), from Korhonen et al. (2002, 2004; vertically shaded), and from Doppler maps (filled). Results of the present paper are plotted with respect to the left y-axis, the other results (lower in number) with respect to the right y-axis.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{4539fig5.ps} \end{figure}$	Figure 5: Time-series fit for the 1999 dataset. Note the continuous change in the amplitude and the practically vanished amplitude at JD 2 451 310; and, that the rotation period of FK Com is 2.4 days.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{4539fig7.ps} \end{figure}$	Figure 7: Modelling the 1999 dataset in 10 segments with light-curve inversion. Left panels show the data with the fits, the corresponding right panels are the maps of the spot filling factor. Note the very small amplitude in the light curve for this time period.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4539fig8.ps} \end{figure}$	Figure 8: Time-series fit for the 1997 dataset. The light variability changes smoothly and is never below 0.1 mag. A sudden change in the light curve shape is seen shortly after JD 2 450 500.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{4539fi10.ps} \end{figure}$	Figure 10: Modelling the 1997 dataset in 10 segments with the light-curve inversion method. Left panels show the data with the fits, the corresponding right panels are the maps of the spot filling factor.
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