Astronomy & Astrophysics

All Figures

$\begin{figure} \par {\includegraphics[width=8.7cm,clip]{4942fig1.eps} } \end{figure}$ Figure 1: EIT images of the erupting filament: a) pre-eruption phase and b) eruption phase. The solid lines indicate the slit positions of time slices shown in Fig. 1. The dashed-line box shows the field of view of Fig. 3. The arrow points to the emerging flux region (EFR) near the filament.
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In the text

$\begin{figure} \par {\includegraphics[width=8.6cm,clip]{4942fig2.eps} } \end{figure}$ Figure 2: Time slices for slit 1 ( upper panel) and slit 2 ( lower panel). The positions of the slits are indicated in Fig. 1. The distance is measured from the northern end of each slit. The black solid lines show the velocity of the filament along the slits. The vertical white lines in the lower panel indicate the reversal points of the oscillation; the solid and dashed lines correspond to the opposite phases.
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In the text

$\begin{figure} \par {\includegraphics[width=8.8cm,clip]{4942fig3.eps} } \end{figure}$ Figure 3: H $\alpha$ wing images at 04:12 UT (panels a) and b)) and at 05:27 UT (panels c) and d)). Panels a) and c) are of the blue wing at -0.8 Å and panels b) and d) are of the red wing at +0.8 Å. Overlaid are 40 DN s^-1 pix^-1 contour at 04:12 UT (panels a) and b)) and at 05:24 UT (panels c) and d)). The arrows show the velocity field on the plane of the sky calculated by correlation tracking of the EIT images. The velocity field is shown only in the region where the EIT count is less than 40 DN s^-1 pix^-1.
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In the text

$\begin{figure} \par {\includegraphics[width=8.7cm,clip]{4942fig1.eps} } \end{figure}$	Figure 1: EIT images of the erupting filament: a) pre-eruption phase and b) eruption phase. The solid lines indicate the slit positions of time slices shown in Fig. 1. The dashed-line box shows the field of view of Fig. 3. The arrow points to the emerging flux region (EFR) near the filament.
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