All Figures

$\begin{figure} \par\includegraphics[width=5cm,clip]{2745f1.ps} \end{figure}$ Figure 1: $R-\theta$ map, close-up of the closed equatorial region (initial condition, t=0) showing the coronal streamer, radial heliocentric distances within $[1,4.4]~R_{\rm s}$ and colatitude $\theta$ within $[40^\circ ,130^\circ ]$ . North is down, South is up. a) Velocity field, together with plasma $\beta$ contours; b) magnetic field lines.
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In the text

$\begin{figure} \par\includegraphics[width=5.5cm,clip]{2745f2.ps} \end{figure}$ Figure 2: Run R, $R-\theta$ map, close-up of the closed equatorial region at t=0.5 showing the coronal streamer, radial heliocentric distances within $[1,4.4]~R_{\rm s}$ and colatitude $\theta$ within $[40^\circ ,130^\circ ]$ . North is down, South is up. From top to bottom: a) velocity field at t=0.5 (14 wave periods), together with contours of $u_\phi$ at [-40,40] km s^-1; b) three selected magnetic field lines, and image of magnetic wave pressure $B_\phi ^2$ at t=0.5 (arbitrary units); c) same three selected magnetic field lines, and image of relative density increase $\delta \rho /\rho$ between time 0 and 0.5: white is 30 $\%$ , black $-30\%$ .
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In the text

$\begin{figure} \par\includegraphics[width=5.5cm,clip]{2745f3.ps} \end{figure}$ Figure 3: Run R. a), b): wave pressure vs. position along loops A and C, one wave period; c): parallel velocity vs. heliocentric distance along equator, at times t=0.1, 0.3, 0.5 (resp. continuous, dotted, dashed). A, B and C indicate the positions of the apex of the loops shown in Fig. 1. Negative velocity means northward flow; d), e): pressure difference vs. position along loops A and C at t = 0.1, 0.3, 0.5. Abscissa starts at north foot-point, so that the excited foot-point is at right in panels a), b), d), e).
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In the text

$\begin{figure} \par\includegraphics[width=5cm,clip]{2745f4.ps} \end{figure}$ Figure 4: Run R. Mass flux estimated as $F= \rho u_\Vert /B$ (see text) vs. position along loops A ( a)) and C ( b)) at t=0.1, 0.3, 0.5 (resp. continuous, dotted, dashed). Abscissa starts at north foot-point, so that the excited foot-point is at right in the figure.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{2745f5.ps} \end{figure}$ Figure 5: Run S1, $R-\theta$ map, close up of the closed equatorial region as in Fig. 2 at t=0.5. From top to bottom: a) velocity field, together with contours of $u_\phi$ at [-40,40] km s^-1; b) three selected magnetic field lines (same as Fig. 1), and image of magnetic wave pressure $B_\phi ^2/2$ ; c) three selected magnetic field lines and image of relative density increase $\delta \rho /\rho$ between time 0 and 0.5: white is larger or equal to 30 $\%$ , black is $-30\%$ . (the actual extremal values in the domain are larger).
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{2745f6.ps} \end{figure}$ Figure 6: Run S1. Wave pressure vs. position along loops A ( a)) and C ( b)), during one wave period; c): gas pressure variation vs. position along loop A, t=0.02,...0.5.
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In the text

$\begin{figure} \par\includegraphics[width=6.1cm,clip]{2745f7.ps} \end{figure}$ Figure 7: Run S1, sample profiles vs. position along loop A, during one wave period around t=0.5. a) Acceleration $-P_{\rm w}'/\rho$ due to wave pressure $P_{\rm w}$ ; b) acceleration due to wave pressure and thermal pressure: $-P_{\rm w}'/\rho-P'/\rho+(P'/\rho)~(t=0)$ (prime denotes derivative with respect to abscissa along loop); c) parallel velocity. Positive parallel velocity or acceleration means southward. Abscissa starts at the north foot-point, so that the excited foot-point is to the right.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{2745f8.ps} \end{figure}$ Figure 8: Run S1. a), b): parallel velocity vs. radial distance along equator and vs. colatitude at inner boundary, at times t=0.1,0.3,0.5 (resp. continuous, dotted, dashed lines); c): wave pressure vs. colatitude at inner boundary. Loops A, B and C are marked for their apex in a) and footpoints in b) and c).
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{2745f9.ps} \end{figure}$ Figure 9: Run S2. a) Parallel velocity vs. colatitude at inner boundary at times t=0.1, 0.3, 0.5 (resp. continuous, dotted, dashed lines); b) wave pressure $B_\phi ^2/2$ vs. colatitude at inner boundary versus colatitude, several profiles during one wave period (t=0.5). Foot-points latitude of loops A, B and C are indicated.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{2745f10.ps} \end{figure}$ Figure 10: Run T2, $R-\theta$ map, close up of the closed equatorial region as in Fig. 4. From top to bottom: a) velocity field, together with contours of $u_\phi$ at [-40,40] km s^-1; b) three selected magnetic field lines, and image of magnetic wave pressure $B_\phi ^2/2$ ; c) three selected magnetic field lines and image of relative density increase $\delta \rho /\rho$ between time 0 and 0.5: white is larger or equal to 10 $\%$ , black is $-10\%$ .
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In the text

$\begin{figure} \par\includegraphics[width=5cm,clip]{2745f11.ps} \end{figure}$ Figure 11: Runs T2 a) and U3 b). Parallel velocity vs. position along loop A, at times t=0.1, 0.3, 0.5 (resp. continuous, dotted, dashed lines).
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{2745f12.ps} \end{figure}$ Figure 12: Parallel velocity vs. time, at apex of loop A for runs T2 a) and U3 b) and c). a) Short time evolution, run T2; b) short time evolution, run U3; c) long time evolution, run U3. Time is given in numerical unit $\tau = 8.4$ h.
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In the text

$\begin{figure} \par\includegraphics[width=5cm,clip]{2745f13.ps} \end{figure}$ Figure 13: Parallel velocity at t=0.5 vs. radial distance along equator, scaling with wave amplitude. a) Continuous line: parallel velocity in run Ra; dotted: parallel velocity in run R, multiplied by 1/4; b) continuous line: parallel velocity in run S1a; dotted: parallel velocity in run S1, multiplied by 1/4.
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In the text

$\begin{figure} \par\includegraphics[width=5.5cm,clip]{2745f14.ps} \end{figure}$ Figure 14: Density vs. colatitude for several runs and at two heliocentric distances: r=1.25 $R_{\rm s}$ (apex of loop A), and $r=2.74~R_{\rm s}$ (apex of loop C). Dotted line: initial profile at t=0. Continuous lines: sample profiles during one wave period at t=0.5.
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In the text

$\begin{figure} \par\includegraphics[width=5cm,clip]{2745f1.ps} \end{figure}$	Figure 1: $R-\theta$ map, close-up of the closed equatorial region (initial condition, t=0) showing the coronal streamer, radial heliocentric distances within $[1,4.4]~R_{\rm s}$ and colatitude $\theta$ within $[40^\circ ,130^\circ ]$ . North is down, South is up. a) Velocity field, together with plasma $\beta$ contours; b) magnetic field lines.
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$\begin{figure} \par\includegraphics[width=5cm,clip]{2745f4.ps} \end{figure}$	Figure 4: Run R. Mass flux estimated as $F= \rho u_\Vert /B$ (see text) vs. position along loops A ( a)) and C ( b)) at t=0.1, 0.3, 0.5 (resp. continuous, dotted, dashed). Abscissa starts at north foot-point, so that the excited foot-point is at right in the figure.
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$\begin{figure} \par\includegraphics[width=6cm,clip]{2745f6.ps} \end{figure}$	Figure 6: Run S1. Wave pressure vs. position along loops A ( a)) and C ( b)), during one wave period; c): gas pressure variation vs. position along loop A, t=0.02,...0.5.
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$\begin{figure} \par\includegraphics[width=6cm,clip]{2745f8.ps} \end{figure}$	Figure 8: Run S1. a), b): parallel velocity vs. radial distance along equator and vs. colatitude at inner boundary, at times t=0.1,0.3,0.5 (resp. continuous, dotted, dashed lines); c): wave pressure vs. colatitude at inner boundary. Loops A, B and C are marked for their apex in a) and footpoints in b) and c).
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$\begin{figure} \par\includegraphics[width=6cm,clip]{2745f9.ps} \end{figure}$	Figure 9: Run S2. a) Parallel velocity vs. colatitude at inner boundary at times t=0.1, 0.3, 0.5 (resp. continuous, dotted, dashed lines); b) wave pressure $B_\phi ^2/2$ vs. colatitude at inner boundary versus colatitude, several profiles during one wave period (t=0.5). Foot-points latitude of loops A, B and C are indicated.
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$\begin{figure} \par\includegraphics[width=5cm,clip]{2745f11.ps} \end{figure}$	Figure 11: Runs T2 a) and U3 b). Parallel velocity vs. position along loop A, at times t=0.1, 0.3, 0.5 (resp. continuous, dotted, dashed lines).
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$\begin{figure} \par\includegraphics[width=6cm,clip]{2745f12.ps} \end{figure}$	Figure 12: Parallel velocity vs. time, at apex of loop A for runs T2 a) and U3 b) and c). a) Short time evolution, run T2; b) short time evolution, run U3; c) long time evolution, run U3. Time is given in numerical unit $\tau = 8.4$ h.
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$\begin{figure} \par\includegraphics[width=5cm,clip]{2745f13.ps} \end{figure}$	Figure 13: Parallel velocity at t=0.5 vs. radial distance along equator, scaling with wave amplitude. a) Continuous line: parallel velocity in run Ra; dotted: parallel velocity in run R, multiplied by 1/4; b) continuous line: parallel velocity in run S1a; dotted: parallel velocity in run S1, multiplied by 1/4.
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$\begin{figure} \par\includegraphics[width=5.5cm,clip]{2745f14.ps} \end{figure}$	Figure 14: Density vs. colatitude for several runs and at two heliocentric distances: r=1.25 $R_{\rm s}$ (apex of loop A), and $r=2.74~R_{\rm s}$ (apex of loop C). Dotted line: initial profile at t=0. Continuous lines: sample profiles during one wave period at t=0.5.
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