All Figures

$\begin{figure} \par\includegraphics[width=6.4cm,clip]{1544Fig1.eps} \end{figure}$ Figure 1: Histogram of ejection velocity for 10⁵ particles of radius in the range 0.1 to 1 mm, ejected during the whole ejection process ( $r_{\rm h} \le 3~{\rm au}$ ) of the 1767 return of comet Tempel-Tuttle.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{1544Fig2.eps}\end{figure}$ Figure 2: Non-gravitational forces acting on a meteoroid. The solar direction is bottom left. The solar radiation is responsible for the solar radiation pressure directed in the opposite direction. The Poynting-Robertson force drags the particle in the direction opposite to its velocity vector. The (diurnal) Yarkovsky-Radzievskii force is produced by the anisotropy of the thermal radiation from the particle and is roughly oriented towards the "morning side'' of the particle (upper left in the figure). The seasonal effect (winter "summer warmer than winter'') has been taken into account by Lyytinen & Van Flandern (2000). (see also Radzievskii 1952; Olsson-Steel 1987; Lyytinen & Van Flandern 2000; Burns et al. 1979).
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In the text

$\begin{figure} \par\includegraphics[width=6.8cm,clip]{1544Fig3.eps}\end{figure}$ Figure 3: Nodes of Leonid meteoroids ejected during the 1767 return of comet 55P/Tempel-Tuttle, selected by the first space criterion $\Delta X$ in 2002 (out of 10⁴ particles in the size range 0.1 to 10 mm). The line represents the trajectory of the Earth in the ecliptic J2000 plane. Scale is in AU. The circle symbolizes the zone where the density of particles is computed (see Sect. 4.5).
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{1544Fig4.eps}\end{figure}$ Figure 4: Nodes of Leonid meteoroids ejected during the 1499 return of comet 55P/Tempel-Tuttle, selected by the (wide) first space criterion $\Delta X$ in 2003. The very perturbed stream is divided into 3 different parts. The computation of $\it ZHR$ value is done only where particles encounter the Earth (coordinates: [0.63; 0.77]). See also Vaubaillon et al. (2003).
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{1544Fig5.eps} \end{figure}$ Figure A.1: Configuration of the view of the nucleus.

In the text

$\begin{figure} \par\includegraphics[width=6.4cm,clip]{1544Fig1.eps} \end{figure}$	Figure 1: Histogram of ejection velocity for 10⁵ particles of radius in the range 0.1 to 1 mm, ejected during the whole ejection process ( $r_{\rm h} \le 3~{\rm au}$ ) of the 1767 return of comet Tempel-Tuttle.
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$\begin{figure} \par\includegraphics[width=6.8cm,clip]{1544Fig3.eps}\end{figure}$	Figure 3: Nodes of Leonid meteoroids ejected during the 1767 return of comet 55P/Tempel-Tuttle, selected by the first space criterion $\Delta X$ in 2002 (out of 10⁴ particles in the size range 0.1 to 10 mm). The line represents the trajectory of the Earth in the ecliptic J2000 plane. Scale is in AU. The circle symbolizes the zone where the density of particles is computed (see Sect. 4.5).
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$\begin{figure} \par\includegraphics[width=7.2cm,clip]{1544Fig4.eps}\end{figure}$	Figure 4: Nodes of Leonid meteoroids ejected during the 1499 return of comet 55P/Tempel-Tuttle, selected by the (wide) first space criterion $\Delta X$ in 2003. The very perturbed stream is divided into 3 different parts. The computation of $\it ZHR$ value is done only where particles encounter the Earth (coordinates: [0.63; 0.77]). See also Vaubaillon et al. (2003).
Open with DEXTER