All Figures

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{3100fig1.eps} \end{figure}$ Figure 1: CAMIRAS images of Saturn and its rings at 20.5 ${\rm\mu m}$ . The effective spatial resolution of 1.4 $^{\prime \prime }$ is plotted on the upper right corner. Ring particles motion is clockwise. The East ansa of the ring and the exit of the shadow are on the left side of the planet.
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In the text

$\begin{figure} \par\includegraphics[width=14.4cm,clip]{3100fig2.eps} \end{figure}$ Figure 2: Radial profiles of Saturn's rings in July 1999 and March 2000. Brightness temperature is given as a function of the distance to Saturn center. Profiles taken on the East and West ansae are overlapping for a better comparison. Error bars represent $\pm$ $0.3~\rm K$ ( $1 \sigma$ ) average uncertainty over the rings. In March 2000, the East ansa is slightly truncated at the edge of the detector array. Vertical dashed lines represent Saturn radius ( $R_{\rm S}=60~330~\rm km$ ) and boundaries of main rings.
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In the text

$\begin{figure} \par\includegraphics[width=14.4cm,clip]{3100fig3.eps} \end{figure}$ Figure 3: Azimuthal brightness temperature profiles of B and C rings in July 1999 and March 2000. Longitude $0^{\circ }$ is located at midnight in the middle of the shadow. The East (morning) ansa is at longitude $90^{\circ }$ , noon at $\pm 180^{\circ }$ and West (afternoon) ansa at longitude $-90^{\circ }$ . Error bars represent $1 \sigma$ uncertainty. Vertical dashed lines represent the shadow limits on the rings. The shadow extent does not change significantly between epochs at the longitudinal scale of this figure. The ellipsoid shape of Saturn was taken into account.
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In the text

$\begin{figure} \par\includegraphics[width=14.4cm,clip]{3100fig4.eps} \end{figure}$ Figure 4: Absorbed fluxes of B and C rings as a function of ring longitude and heating sources for Bond albedo $A_{\rm V}=0.5$ and f=2 at July 1999 epoch. (- $\cdot \cdot \cdot$ ) F₁, (- $\cdot$ -) F₁+F₃, (- -) F₁+F₃+F₄, (...) F₁+F₃+F₄+infrared neighbours, (solid line) F₁+F₂+F₃+F₄ +infrared neighbours. Longitude is zero at midnight; West ansa (W) is located at $-90^{\circ }$ and East ansa (E) at $90^{\circ }$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{3100fig5.eps} \par\end{figure}$ Figure 5: Azimuthal variation of the surface temperature as a function of thermal inertia $\Gamma$ ( ${\rm J ~m^{-2}~ K^{-1} ~s^{-1/2}}$ ). The particle is located at a=84 000 km from Saturn, $A_{\rm V}=0.5$ , f=2 and $\rho =918$ ${\rm kg~m^{-3}}$ . Calculations are made for the viewing geometry of the July 1999 epoch. In this case, $T_0=92.6~\rm K$ and $C_{\rm H}=783.7$ ${\rm J~~kg^{-1}~K^{-1}}$ . All incident fluxes but F₂ have been included.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{3100fig6.eps} \end{figure}$ Figure 6: Best fit of the B ring data of Froidevaux et al. (1981) obtained with our eclipse model for f=2. Thermal inertia is $\Gamma =16^{+14}_{-11}$ ${\rm J ~m^{-2}~ K^{-1} ~s^{-1/2}}$ and Bond albedo $A_{\rm V}=0.48^{+0.04}_{-0.07}$ at 3 $\sigma$ . At the epoch $B=12.8^{\circ }$ , $B'=10^{\circ }$ and the phase angle is $6.3^{\circ }$ on the East ansa. "Max'' and "Min'' show the temperature for the limit values $\Gamma$ and $A_{\rm V}=0.48$ .
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In the text

$\begin{figure} \par\includegraphics[width=14.4cm,clip]{3100fig7.eps} \end{figure}$ Figure 7: Brightness temperature azimuthal profile of the B ring at range a=105 000 km ( $1.74 R_{\rm S}$ ) in July 1999 and March 2000. Best fits (3 $\sigma$ ) are represented in case of: (E) fit with east ansa data only, (E+W) fit with east and west ansae data.
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In the text

$\begin{figure} \par\includegraphics[width=14.4cm,clip]{3100fig8.eps} \end{figure}$ Figure 8: Best fits of brightness temperature azimuthal profile of the C ring at range a=84 000 km ( $1.39 R_{\rm S}$ ) in July 1999 and March 200. See Fig. 7 for details.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{3100fig9.eps} \end{figure}$ Figure 9: Thermal inertias $\Gamma$ and Bond albedos $A_{\rm V}$ of B and C rings. Solutions are found by using data from: (triangle) CAMIRAS, July 1999 with East ansa only; (square) CAMIRAS, July 1999 with both ansae; (cross) CAMIRAS, March 2000 with East ansa only; (full circle) CAMIRAS, March 2000 with both ansae; (losange) Froidevaux 1981(see Fig. 6). Errors bars are given at $3 \sigma$ level.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{3100fig1.eps} \end{figure}$	Figure 1: CAMIRAS images of Saturn and its rings at 20.5 ${\rm\mu m}$ . The effective spatial resolution of 1.4 $^{\prime \prime }$ is plotted on the upper right corner. Ring particles motion is clockwise. The East ansa of the ring and the exit of the shadow are on the left side of the planet.
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$\begin{figure} \par\includegraphics[width=14.4cm,clip]{3100fig7.eps} \end{figure}$	Figure 7: Brightness temperature azimuthal profile of the B ring at range a=105 000 km ( $1.74 R_{\rm S}$ ) in July 1999 and March 2000. Best fits (3 $\sigma$ ) are represented in case of: (E) fit with east ansa data only, (E+W) fit with east and west ansae data.
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$\begin{figure} \par\includegraphics[width=14.4cm,clip]{3100fig8.eps} \end{figure}$	Figure 8: Best fits of brightness temperature azimuthal profile of the C ring at range a=84 000 km ( $1.39 R_{\rm S}$ ) in July 1999 and March 200. See Fig. 7 for details.
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