All Figures

$\begin{figure} \par\includegraphics[width=6.8cm,clip]{3348fg1.ps} \end{figure}$ Figure 1: Definition of the magnetic field orientation angle $\theta$ for the modeled sinistral filaments, where the dominant photospheric positive polarities are located in x>0. $\theta <0$ (resp. >0) and the label IP (resp. NP) correspond to "inverse'' (resp. "normal'') polarity configurations.
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In the text

$\begin{figure} \par\includegraphics[width=17.8cm,clip]{3348fg2.ps} \end{figure}$ Figure 2: Color-coded distribution of magnetic dips within the Nov. 04, 1999 quiescent filament, located at E34 S17 (modeled in Aulanier et al. 2000). Only the central position of the dips (i.e. where B_z=0) are shown, as open circles to highlight different structures along the line-of-sight. Left column: amplitude of the magnetic field $\vert\vert\vec{B}\vert\vert$ . Note that in the prominence body, $<\vert\vert\vec{B}\vert\vert>~ \sim 2.5 {-} 3$ G. Right column: angle $\theta$ made between ${\vec B}$ and the mean axis y of the inversion line. $\theta <0$ (resp. >0) refer to "inverse'' (resp. "normal'') polarity fields. Top row: scatter plots of $\vert\vert\vec{B}\vert\vert$ and $\theta$ versus altitude within the whole prominence. The colors are changing from purple to red as $\vert\vert\vec{B}\vert\vert$ and $\theta$ increase (for the latter, yellow corresponds to $\theta =0$ ); the same color-codes are used in all the panels. Lower rows: 3D projections of the prominence dips (same color-coding as for the top row) as viewed on the limb along the y axis (second row), perpendicularly to the prominence, along the x axis (third row) and from above along the z axis, as for a filament located at disc center (bottom row). Note that the apparent vertical and curved structures within the prominence are an artifact of the discretized calculation of dips.
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In the text

$\begin{figure} \par\includegraphics[width=17.8cm,clip]{3348fg3.ps} \end{figure}$ Figure 3: Same as Fig. 2, but for the Sep. 25, 1996 intermediate filament located at E5 S2 (modeled in Aulanier et al. 1999). Note that $<\vert\vert\vec{B}\vert\vert>~ \sim 13 {-} 15$ G in the prominence body.
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In the text

$\begin{figure} \par\includegraphics[width=17.8cm,clip]{3348fg4.ps} \end{figure}$ Figure 4: Same as Fig. 2, but for the May 05, 2000 plage filament located at E17 S21 within a decaying active region (modeled in Aulanier & Schmieder 2002). Note that $<\vert\vert\vec{B}\vert\vert>~ \sim 35{-} 45$ G in the prominence body.
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In the text

$\begin{figure} \par\includegraphics[width=6.8cm,clip]{3348fg1.ps} \end{figure}$	Figure 1: Definition of the magnetic field orientation angle $\theta$ for the modeled sinistral filaments, where the dominant photospheric positive polarities are located in x>0. $\theta <0$ (resp. >0) and the label IP (resp. NP) correspond to "inverse'' (resp. "normal'') polarity configurations.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=17.8cm,clip]{3348fg3.ps} \end{figure}$	Figure 3: Same as Fig. 2, but for the Sep. 25, 1996 intermediate filament located at E5 S2 (modeled in Aulanier et al. 1999). Note that $<\vert\vert\vec{B}\vert\vert>~ \sim 13 {-} 15$ G in the prominence body.
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$\begin{figure} \par\includegraphics[width=17.8cm,clip]{3348fg4.ps} \end{figure}$	Figure 4: Same as Fig. 2, but for the May 05, 2000 plage filament located at E17 S21 within a decaying active region (modeled in Aulanier & Schmieder 2002). Note that $<\vert\vert\vec{B}\vert\vert>~ \sim 35{-} 45$ G in the prominence body.
Open with DEXTER