All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{9086fig1.ps}\end{figure}$ Figure 1: Part of the MDI magnetogram of the active region NOAA 9366 that was used for the magnetic field extrapolation. White (Black) stands for positive (negative) line of sight photospheric magnetic fields. The active region is characterized by two dominant polarities.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{9086fig2.ps}\end{figure}$ Figure 2: Field lines of the magnetic field extrapolation that were chosen to represent the active region loops. Most of the loops connect the two dominant polarities. The axes represent the pixel size of the magnetograph.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{9086fig3.ps} \end{figure}$ Figure 3: Averages of the magnetic field (panel a), the magnetic field energy (panel b), the maximal loop cross section (panel c), the resistance (panel d), and the average volumetric heating (panel e), as a function of the loop lengths. Panel f) shows the scatter plot between the mean volumetric heating and the mean magnetic energy along the loops. In the first two panels, a linear fit, in logarithmic unit was completed for loop lengths in the range 50-100 Mm.
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In the text

$\begin{figure} \par\includegraphics[width=8.7cm,clip]{9086fig4.ps} \end{figure}$ Figure 4: Mean volumetric heating (solid line) and mean magnetic field square (dashed line) as functions of height above the active region shown in Fig. 1.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{9086fig5.ps} \end{figure}$ Figure 5: Maximum loop width (cross section square root) versus mean heating along the loops. The loop points are separated into 2 panels according to their length.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{9086fig6.ps} \end{figure}$ Figure 6: Heating flux as a function of the average loop footpoint normal magnetic field. Each diamond in this plot represents a single loop.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{9086fig7.ps} \end{figure}$ Figure 7: Statistics of the loop heating asymmetry are shown in the panels of the first row. Panel a) shows the ratios of the heating length scales over loop lengths. Panel b) shows the heating rate at each footpoint. Four examples of loops geometry (panel c) and heating (panel d) along their length showing their asymmetry. The thick parts of the curves correspond to the chromosphere.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{9086fig8.ps} \end{figure}$ Figure 8: Correlations derived from the stable hydrostatic solutions for half loops. Panel a) shows the maximum temperatures as a function of the loop lengths. Panel b) shows the footpoint pressure as a function of the loop lengths. Panel c) shows the maximum temperature as a function of the footpoint pressure and panel d) the maximum temperature as a function of the mean heating.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{9086fig9.ps} \end{figure}$ Figure 9: Panels a) and b) show AR 9366, observed in the 171 Å and 284 Å EIT passbands respectively. Panels c) and d) show the computed emission in 171 and 284 based on the hydrostatic solution loops.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{9086fig1.ps}\end{figure}$	Figure 1: Part of the MDI magnetogram of the active region NOAA 9366 that was used for the magnetic field extrapolation. White (Black) stands for positive (negative) line of sight photospheric magnetic fields. The active region is characterized by two dominant polarities.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{9086fig2.ps}\end{figure}$	Figure 2: Field lines of the magnetic field extrapolation that were chosen to represent the active region loops. Most of the loops connect the two dominant polarities. The axes represent the pixel size of the magnetograph.
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$\begin{figure} \par\includegraphics[width=8.7cm,clip]{9086fig4.ps} \end{figure}$	Figure 4: Mean volumetric heating (solid line) and mean magnetic field square (dashed line) as functions of height above the active region shown in Fig. 1.
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$\begin{figure} \par\includegraphics[width=9cm,clip]{9086fig5.ps} \end{figure}$	Figure 5: Maximum loop width (cross section square root) versus mean heating along the loops. The loop points are separated into 2 panels according to their length.
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$\begin{figure} \par\includegraphics[width=9cm,clip]{9086fig6.ps} \end{figure}$	Figure 6: Heating flux as a function of the average loop footpoint normal magnetic field. Each diamond in this plot represents a single loop.
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$\begin{figure} \par\includegraphics[width=9cm,clip]{9086fig7.ps} \end{figure}$	Figure 7: Statistics of the loop heating asymmetry are shown in the panels of the first row. Panel a) shows the ratios of the heating length scales over loop lengths. Panel b) shows the heating rate at each footpoint. Four examples of loops geometry (panel c) and heating (panel d) along their length showing their asymmetry. The thick parts of the curves correspond to the chromosphere.
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$\begin{figure} \par\includegraphics[width=9cm,clip]{9086fig8.ps} \end{figure}$	Figure 8: Correlations derived from the stable hydrostatic solutions for half loops. Panel a) shows the maximum temperatures as a function of the loop lengths. Panel b) shows the footpoint pressure as a function of the loop lengths. Panel c) shows the maximum temperature as a function of the footpoint pressure and panel d) the maximum temperature as a function of the mean heating.
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$\begin{figure} \par\includegraphics[width=9cm,clip]{9086fig9.ps} \end{figure}$	Figure 9: Panels a) and b) show AR 9366, observed in the 171 Å and 284 Å EIT passbands respectively. Panels c) and d) show the computed emission in 171 and 284 based on the hydrostatic solution loops.
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