All Figures

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{1373_f1.ps}\end{figure}$ Figure 1: Observed (dots) and synthetic (full lines) light and temperature curves of VY Ari. The B-V curve is also shown in the lower box with the solution superimposed for comparison. A schematic map of the starspot distribution, as seen at two different rotational phases, is also shown.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{1373_f2.ps}\end{figure}$ Figure 2: Observed (dots) and synthetic (full lines) light and temperature curves of IM Peg. The B-V curve is also shown in the lower box with the solution superimposed for comparison. A schematic map of the starspot distribution, as seen at two different rotational phases, is also shown.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{1373_f3.ps}\end{figure}$ Figure 3: Observed (dots) and synthetic (full lines) temperature and light curves of HK Lac. The B-V curve is also shown in the lower box with the solution superimposed for comparison. A schematic map of the starspot distribution, as seen at two different rotational phases, is also shown.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{1373_f4.ps}\end{figure}$ Figure 4: Continuum flux at $\lambda 6190$ Å for Kurucz spectra (squares), NextGen spectra (asterisks) with $\log g=2.5$ and for black-body radiation (full line) as a function of $T_{\rm eff}$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{1373_f5.ps}\end{figure}$ Figure 5: V-band flux for Kurucz spectra (squares), NextGen spectra (asterisks) with $\log g=2.5$ and for black-body radiation (full line) as a function of $T_{\rm eff}$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{1373_f6.ps}\end{figure}$ Figure 6: Examples of synthetic curves for three spot temperatures (lines) superimposed on the V light curve of VY Ari (dots). The three curves are practically indistinguishable, notwithstanding the large differences in spots temperature that are compensated by spot sizes. In the lower panel is shown the $\chi$ -square as a function of the relative spot temperature $T_{\rm sp}/T_{\rm ph}$ .
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{1373_f7.ps}\end{figure}$ Figure 7: Grids of solutions for VY Ari. The filled circles represent the solutions for light curve, while the filled diamonds represent the solutions for temperature curve. The hatched area, in each box, is the locus of the allowed solutions accounting for data errors.
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In the text

$\begin{figure} \par\includegraphics[width=7.15cm]{1373_f8.ps}\end{figure}$ Figure 8: Grids of solutions for IM Peg. The filled circles represent the solutions for light curve, while the filled diamonds represent the solutions for temperature curve. The hatched area, in each box, is the locus of the allowed solutions accounting for data errors.
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In the text

$\begin{figure} \par\includegraphics[width=7.15cm,clip]{1373_f9.ps}\end{figure}$ Figure 9: Grids of solutions for HK Lac. The filled circles represent the solutions for light curve, while the filled diamonds represent the solutions for temperature curve. The hatched area, in each box, is the locus of the allowed solutions accounting for data errors.
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In the text

$\begin{figure} \par\includegraphics[width=6.9cm,clip]{1373_fa1.ps}\end{figure}$ Figure A.1: Illustrative example of a line pair (V I $\lambda 6199$ -Fe I $\lambda 6200$ ) in spectra of standard stars with temperatures typical of the photosphere of an active early-K star (upper plot) and of a starspot (lower plot). The line-depth of both lines and the continuum fluxes, used in Eq. (A.1)-(A.4), are also indicated.

In the text

$\begin{figure} \par\includegraphics[width=7.15cm,clip]{1373_fa2.ps}\end{figure}$ Figure A.2: Observed (dots) and synthesized LDRs (dashed lines) for HK Lac. The LDR curves corrected for the small offsets are displayed with full lines.

In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{1373_f1.ps}\end{figure}$	Figure 1: Observed (dots) and synthetic (full lines) light and temperature curves of VY Ari. The B-V curve is also shown in the lower box with the solution superimposed for comparison. A schematic map of the starspot distribution, as seen at two different rotational phases, is also shown.
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$\begin{figure} \par\includegraphics[width=7.2cm,clip]{1373_f2.ps}\end{figure}$	Figure 2: Observed (dots) and synthetic (full lines) light and temperature curves of IM Peg. The B-V curve is also shown in the lower box with the solution superimposed for comparison. A schematic map of the starspot distribution, as seen at two different rotational phases, is also shown.
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$\begin{figure} \par\includegraphics[width=7.2cm,clip]{1373_f3.ps}\end{figure}$	Figure 3: Observed (dots) and synthetic (full lines) temperature and light curves of HK Lac. The B-V curve is also shown in the lower box with the solution superimposed for comparison. A schematic map of the starspot distribution, as seen at two different rotational phases, is also shown.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{1373_f4.ps}\end{figure}$	Figure 4: Continuum flux at $\lambda 6190$ Å for Kurucz spectra (squares), NextGen spectra (asterisks) with $\log g=2.5$ and for black-body radiation (full line) as a function of $T_{\rm eff}$ .
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{1373_f5.ps}\end{figure}$	Figure 5: V-band flux for Kurucz spectra (squares), NextGen spectra (asterisks) with $\log g=2.5$ and for black-body radiation (full line) as a function of $T_{\rm eff}$ .
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$\begin{figure} \par\includegraphics[width=7.2cm,clip]{1373_f6.ps}\end{figure}$	Figure 6: Examples of synthetic curves for three spot temperatures (lines) superimposed on the V light curve of VY Ari (dots). The three curves are practically indistinguishable, notwithstanding the large differences in spots temperature that are compensated by spot sizes. In the lower panel is shown the $\chi$ -square as a function of the relative spot temperature $T_{\rm sp}/T_{\rm ph}$ .
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$\begin{figure} \par\includegraphics[width=7cm,clip]{1373_f7.ps}\end{figure}$	Figure 7: Grids of solutions for VY Ari. The filled circles represent the solutions for light curve, while the filled diamonds represent the solutions for temperature curve. The hatched area, in each box, is the locus of the allowed solutions accounting for data errors.
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$\begin{figure} \par\includegraphics[width=7.15cm]{1373_f8.ps}\end{figure}$	Figure 8: Grids of solutions for IM Peg. The filled circles represent the solutions for light curve, while the filled diamonds represent the solutions for temperature curve. The hatched area, in each box, is the locus of the allowed solutions accounting for data errors.
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$\begin{figure} \par\includegraphics[width=7.15cm,clip]{1373_f9.ps}\end{figure}$	Figure 9: Grids of solutions for HK Lac. The filled circles represent the solutions for light curve, while the filled diamonds represent the solutions for temperature curve. The hatched area, in each box, is the locus of the allowed solutions accounting for data errors.
Open with DEXTER