Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=8.1cm,clip]{Gc101_f1.ps} \end{figure}$ Figure 1: Comparison of 2001 XR31 with R-type MBAs (taken from Bus 1999) in the visible region. The mean V-type and (3155) Lee are also shown (both from Bus 1999).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.1cm,clip]{Gc101_f2.ps} \end{figure}$ Figure 2: Comparison of 2001 XR31 with R-type asteroids. On the same plot, (4) Vesta and (3155) Lee are also shown. The NIR of (1904) Massevitch and (3155) Lee are from SMASSIR (Burbine et al. 1997), while the NIR of (349) Dembowska is from 52-Color survey (Bell et al. 1988).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=11cm,clip]{Gc101_f3.ps} \end{figure}$ Figure 3: Distribution of ejecta from (349) Dembowska in the (a, e) plane, for catastrophic disruption and cratering event. In the latter case, the ejection cone is oriented along the direction of motion of (349) Dembowska. In both cases, the fragments are generated with a uniform distribution of velocity modules between 0 and 0.15 km s^-1, and for (349) Dembowska's true anomaly of 90 deg (see text).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.1cm,clip]{Gc101_f1.ps} \end{figure}$	Figure 1: Comparison of 2001 XR31 with R-type MBAs (taken from Bus 1999) in the visible region. The mean V-type and (3155) Lee are also shown (both from Bus 1999).
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=-90,width=8.1cm,clip]{Gc101_f2.ps} \end{figure}$	Figure 2: Comparison of 2001 XR31 with R-type asteroids. On the same plot, (4) Vesta and (3155) Lee are also shown. The NIR of (1904) Massevitch and (3155) Lee are from SMASSIR (Burbine et al. 1997), while the NIR of (349) Dembowska is from 52-Color survey (Bell et al. 1988).
Open with DEXTER