All Figures

$\begin{figure} \par\includegraphics[width=8.8cm]{1428fig1.eps} \end{figure}$ Figure 1: The normalized system efficiencies (NSEs). The solid curve indicates the NSE of the HDTV spectroscopic observational system onboard with the grating of 600 grooves/mm (blaze 300 nm), calibrated with Jupiter.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1428fig2.eps}\end{figure}$ Figure 2: Time variation of the spectra of the representative Leonid meteor observed at ${\rm03^{h}}$ ${\rm 47^{m}}$ ${\rm 54^{s}}$ UT on November 19, 2002. The time interval is 0.033 s. The emissions around 300 nm were out of the field of view before 0.165 s.
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In the text

$\begin{figure} \par\includegraphics[width=12cm]{1428fig3.eps}\end{figure}$ Figure 3: An example of the reduced spectrum (narrow line) at 0.165 s. The meteor spectrum was obtained by subtracting the blackbody radiation from the observed spectrum. Dotted lines are the best fit models by neutral atomic emissions of 358, 374, 383, 404, 423, 438, 518 and 589 nm. The excitation temperature of this frame is $5500~{\rm K}$ and the blackbody temperature is $5250 \pm 250~{\rm K}$ .
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In the text

$\begin{figure} \includegraphics[width=12cm,clip]{1428fig4.eps}\end{figure}$ Figure 4: Time variations of the excitation temperature (thick line), blackbody temperature (thin line) and electron density (dotted line). The 374 nm (FeI) and 383 nm (MgI, FeI) lines were saturated at $t = 0.264~{\rm s}$ and $t =0.297~{\rm s}$ so that the derived exciting temperatures cannot be used for interpretation.
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In the text

$\begin{figure} \par\includegraphics[width=12cm]{1428fig5.eps}\end{figure}$ Figure 5: Time variation of the abundances of Mg, Fe, Ca and Na relative to Mg. The solar abundances (Anders & Grevesse 1989) of Fe, Ca, Na and Mg are shown by the horizontal lines. The 374 nm (FeI) and 383 nm (MgI, FeI) lines were saturated by the strong meteor emissions at $t = 0.264~{\rm s}$ and $t =0.297~{\rm s}$ .
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In the text

$\begin{figure} \par\includegraphics[width=12cm]{1428fig6.eps}\end{figure}$ Figure 6: The abundances of the metallic elements Fe, Ca and Na relative to Mg vs. the excitation temperature.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{1428fig1.eps} \end{figure}$	Figure 1: The normalized system efficiencies (NSEs). The solid curve indicates the NSE of the HDTV spectroscopic observational system onboard with the grating of 600 grooves/mm (blaze 300 nm), calibrated with Jupiter.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1428fig2.eps}\end{figure}$	Figure 2: Time variation of the spectra of the representative Leonid meteor observed at ${\rm03^{h}}$ ${\rm 47^{m}}$ ${\rm 54^{s}}$ UT on November 19, 2002. The time interval is 0.033 s. The emissions around 300 nm were out of the field of view before 0.165 s.
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$\begin{figure} \includegraphics[width=12cm,clip]{1428fig4.eps}\end{figure}$	Figure 4: Time variations of the excitation temperature (thick line), blackbody temperature (thin line) and electron density (dotted line). The 374 nm (FeI) and 383 nm (MgI, FeI) lines were saturated at $t = 0.264~{\rm s}$ and $t =0.297~{\rm s}$ so that the derived exciting temperatures cannot be used for interpretation.
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$\begin{figure} \par\includegraphics[width=12cm]{1428fig5.eps}\end{figure}$	Figure 5: Time variation of the abundances of Mg, Fe, Ca and Na relative to Mg. The solar abundances (Anders & Grevesse 1989) of Fe, Ca, Na and Mg are shown by the horizontal lines. The 374 nm (FeI) and 383 nm (MgI, FeI) lines were saturated by the strong meteor emissions at $t = 0.264~{\rm s}$ and $t =0.297~{\rm s}$ .
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$\begin{figure} \par\includegraphics[width=12cm]{1428fig6.eps}\end{figure}$	Figure 6: The abundances of the metallic elements Fe, Ca and Na relative to Mg vs. the excitation temperature.
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