All Figures

$\begin{figure} \par\includegraphics[width=8.8cm]{9058fig1.eps} %\end{figure}$ Figure 1: Time series of H $\alpha$ profiles for LQ Hya in April-May 2000 sorted in phase order. The non-active template built up with a spectrum of the non-active, slowly-rotating K2 V star HD 3765 is shown by a dash-dotted line at the bottom. The vertical dotted lines mark the integration interval for the raw H $\alpha$ equivalent width ( ${\it EW}_{\rm H\alpha }$ ).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{9058fig2.eps} \end{figure}$ Figure 2: From top to bottom. The computed electron density $n_{\rm e}$ (cm^-3), the flux ratio between the red and the blue peaks, and the peak separation in Å against the rotational phase.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{9058fig3.eps} \end{figure}$ Figure 3: Top panel: V light curve contemporaneous to the spectra. Middle panels: rotational modulation of the raw H $\alpha$ equivalent width ( ${\it EW}_{\rm H\alpha }$ , open circles) and of the residual H $\alpha$ EW ( $\Delta {\it EW}_{\rm H\alpha }$ , filled circles). Bottom panel: velocity shift between H $\alpha$ emission and photospheric lines both for observed (open circles) and residual spectra (filled circles). The continuous lines in the middle and bottom panels represent the best fit of our 3-plage model (cf. Fig. 4), while the dotted lines represent the result of our 2-plage model.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=2cm,clip]{9058f4a.eps}\hspace{0.... ...ps}\hspace{0.4cm} \includegraphics[width=2cm,clip]{9058f4i.eps} }\end{figure}$ Figure 4: Schematic representation of the surface features of LQ Hya in the chromosphere as reconstructed by the 2-plage ( top) and by the 3-plage models ( middle) and in the photosphere ( bottom). In these maps, the star is rotating counterclockwise. Dominant features are found at similar longitudes at both chromospheric and photospheric levels.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{9058fig1.eps} %\end{figure}$	Figure 1: Time series of H $\alpha$ profiles for LQ Hya in April-May 2000 sorted in phase order. The non-active template built up with a spectrum of the non-active, slowly-rotating K2 V star HD 3765 is shown by a dash-dotted line at the bottom. The vertical dotted lines mark the integration interval for the raw H $\alpha$ equivalent width ( ${\it EW}_{\rm H\alpha }$ ).
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$\begin{figure} \par\includegraphics[width=8.8cm]{9058fig2.eps} \end{figure}$	Figure 2: From top to bottom. The computed electron density $n_{\rm e}$ (cm^-3), the flux ratio between the red and the blue peaks, and the peak separation in Å against the rotational phase.
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$\begin{figure} \par\mbox{\includegraphics[width=2cm,clip]{9058f4a.eps}\hspace{0.... ...ps}\hspace{0.4cm} \includegraphics[width=2cm,clip]{9058f4i.eps} }\end{figure}$	Figure 4: Schematic representation of the surface features of LQ Hya in the chromosphere as reconstructed by the 2-plage ( top) and by the 3-plage models ( middle) and in the photosphere ( bottom). In these maps, the star is rotating counterclockwise. Dominant features are found at similar longitudes at both chromospheric and photospheric levels.
Open with DEXTER