All Figures

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3062_f1.ps} \end{figure}$ Figure 1: Full disk 87 GHz image (or map) obtained at Metsähovi on May 12, 1998. The three lowest radio contours 0, 100, 200 K above the quiet Sun level (7200 K) are shown. Areas with larger enhancement are shown in gray scale only. The high latitude ETR close to the South Pole is shown in Fig. 4 also.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{3062_f2.ps} \end{figure}$ Figure 2: The ETR maximum position R and the intensity contours {k_n}.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3062_f3.ps} \end{figure}$ Figure 3: An example of the brightness distributions over the solar disk, obtained on May 12, 1998. A): corresponds to the CaII(k₃) solar image, B): to the H $_{\alpha }$ solar image. r/R is the relative distance from the solar center, and each dot corresponds to one brightness measurement. The fitted functions f(r/R) are shown by the solid curves.
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In the text

$\begin{figure} \par\includegraphics[width=14.3cm,clip]{3062_f4.eps} \end{figure}$ Figure 4: Details of the CaII(k₃) and H $_{\alpha }$ intensitygrams and SOHO/MDI magnetograms with superposed radio contours, and relations between the average radio brightness and other wavelength data (see the main text for explanations).
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{3062_f5.eps} \end{figure}$ Figure 5: Relation between the average radio brightness and the average CaII(k₃) brightness (with error bars) for the ETR in Fig. 4.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{3062_f6.eps} \end{figure}$ Figure 6: The change in the maximal brightness and the maximal magnetic field strength as a function of the ETR intensity contour or area. A): CaII, B): H $_{\alpha }$ , C): SOHO/MDI magnetic field strength, C1): enlargement of C) in the magnetic field strength interval from 0 to 100 Gauss.
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In the text

$\begin{figure} \par\hspace*{1.4cm}\includegraphics[width=15cm,clip]{3062_f7.eps} \end{figure}$ Figure 7: The change in the average brightness and the average magnetic field strength as a function of the ETR intensity contour area. A): radio, B): CaII, C): H $_{\alpha }$ , D): SOHO/MDI magnetic field strength.
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In the text

$\begin{figure} \par\includegraphics[width=10cm,clip]{3062f8.eps} \end{figure}$ Figure 8: Relations between the changes in the average surface brightness of radio, CaII(k₃) and H $_{\alpha }$ regions. The two highest intensities are from sunspot regions, selected for comparison.
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In the text

$\begin{figure} \par\includegraphics[width=10cm,clip]{3062f9.eps} \end{figure}$ Figure 9: The correlation between the maximal A) and the average B) CaII(k₃) and H $_{\alpha }$ brightnesses in the enhanced radio temperature regions.
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In the text

$\begin{figure} \par\includegraphics[width=10.5cm,clip]{3062f10.eps} \end{figure}$ Figure 10: Relations between the variations of { $m_{{\rm av}n}$ } and { $r_{{\rm av}n}$ } A); { $Ca_{{\rm av}n}$ } B); { $H_{{\rm av}n}$ } C).
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{3062f11.eps} \end{figure}$ Figure 11: Relations between the maximal CaII(k₃) A) and H $_{\alpha }$ B) brightness features and maximal magnetic field strength structures. Figures A1) and B1) are enlargements of the central parts of Figs. A) and B).
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3062_f1.ps} \end{figure}$	Figure 1: Full disk 87 GHz image (or map) obtained at Metsähovi on May 12, 1998. The three lowest radio contours 0, 100, 200 K above the quiet Sun level (7200 K) are shown. Areas with larger enhancement are shown in gray scale only. The high latitude ETR close to the South Pole is shown in Fig. 4 also.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{3062_f2.ps} \end{figure}$	Figure 2: The ETR maximum position R and the intensity contours {k_n}.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3062_f3.ps} \end{figure}$	Figure 3: An example of the brightness distributions over the solar disk, obtained on May 12, 1998. A): corresponds to the CaII(k₃) solar image, B): to the H $_{\alpha }$ solar image. r/R is the relative distance from the solar center, and each dot corresponds to one brightness measurement. The fitted functions f(r/R) are shown by the solid curves.
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$\begin{figure} \par\includegraphics[width=14.3cm,clip]{3062_f4.eps} \end{figure}$	Figure 4: Details of the CaII(k₃) and H $_{\alpha }$ intensitygrams and SOHO/MDI magnetograms with superposed radio contours, and relations between the average radio brightness and other wavelength data (see the main text for explanations).
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$\begin{figure} \par\includegraphics[width=7cm,clip]{3062_f5.eps} \end{figure}$	Figure 5: Relation between the average radio brightness and the average CaII(k₃) brightness (with error bars) for the ETR in Fig. 4.
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$\begin{figure} \par\includegraphics[width=15cm,clip]{3062_f6.eps} \end{figure}$	Figure 6: The change in the maximal brightness and the maximal magnetic field strength as a function of the ETR intensity contour or area. A): CaII, B): H $_{\alpha }$ , C): SOHO/MDI magnetic field strength, C1): enlargement of C) in the magnetic field strength interval from 0 to 100 Gauss.
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$\begin{figure} \par\hspace*{1.4cm}\includegraphics[width=15cm,clip]{3062_f7.eps} \end{figure}$	Figure 7: The change in the average brightness and the average magnetic field strength as a function of the ETR intensity contour area. A): radio, B): CaII, C): H $_{\alpha }$ , D): SOHO/MDI magnetic field strength.
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$\begin{figure} \par\includegraphics[width=10cm,clip]{3062f8.eps} \end{figure}$	Figure 8: Relations between the changes in the average surface brightness of radio, CaII(k₃) and H $_{\alpha }$ regions. The two highest intensities are from sunspot regions, selected for comparison.
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$\begin{figure} \par\includegraphics[width=10cm,clip]{3062f9.eps} \end{figure}$	Figure 9: The correlation between the maximal A) and the average B) CaII(k₃) and H $_{\alpha }$ brightnesses in the enhanced radio temperature regions.
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$\begin{figure} \par\includegraphics[width=10.5cm,clip]{3062f10.eps} \end{figure}$	Figure 10: Relations between the variations of { $m_{{\rm av}n}$ } and { $r_{{\rm av}n}$ } A); { $Ca_{{\rm av}n}$ } B); { $H_{{\rm av}n}$ } C).
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$\begin{figure} \par\includegraphics[width=16cm,clip]{3062f11.eps} \end{figure}$	Figure 11: Relations between the maximal CaII(k₃) A) and H $_{\alpha }$ B) brightness features and maximal magnetic field strength structures. Figures A1) and B1) are enlargements of the central parts of Figs. A) and B).
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