All Figures

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{9069fig1.eps}\par\includegraphics[width=6.7cm,clip]{9069fig2.eps}\end{figure}$ Figure 1: The trajectories of the Ulysses and Cassini spacecraft. Ulysses was launched in 1990 and orbits the Sun now for the third time. Shown is Ulysses´ first orbit. Cassini was launched in 1997 and reached Saturn in 2004. Source: http://helio.estec.esa.nl/ulysses/ and http://saturn.jpl.nasa.gov/home/index.cfm.
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In the text

$\begin{figure} \par\includegraphics[width=6.8cm,clip]{9069fig3.eps}\end{figure}$ Figure 2: The latitudinal structure of the solar wind velocity $f_{\rm\Theta } {v_{\rm0}}$ , see Eq. (5) for solar minimum conditions.
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In the text

$\begin{figure} \par\includegraphics[width=15.7cm,clip]{9069fig4.eps}\end{figure}$ Figure 3: Measurements of the differential electron intensity around 1 MeV from the 4 spacecraft Voyager (1 and 2), Pioneer 11, and Cassini. For comparison, measurements of Pioneer 10 and Cassini at Jupiter are shown. Open symbols stand for measurements at Saturn and filled symbols for those at Jupiter. The first two panels refer to inbound measurements of the Kronian magnetosphere at a distance of about 5 and 11 $R_{\rm s}$ . The right panel is for a distance of approximately 20 $R_{\rm s}$ , which for Voyager 2 and Pioneer 11 corresponds to their crossing distance of the Kronian magnetopause. The Voyager 1 and Cassini data points are measurements inside the Kronian magnetosphere. Pioneer 10 measurements refer to a distance of about 3 $R_{\rm j}$ , which is inside the Jovian magnetosphere. The upper Cassini data point in the right panel determines the location where Cassini entered the Jovian magnetosphere, which was at a distance of about 200 $R_{\rm j}$ , whereas the lower data point is equivalent to the spacecraft's closest approach to Jupiter of about 140 $R_{\rm j}$ . ( $R_{\rm j}=71~400$ km, $R_{\rm s}=60~330$ km).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{9069fig5.eps}\end{figure}$ Figure 4: The computed electron intensities (normalized to the galactic source) along the Cassini (solid line) and Ulysses (dashed line) trajectories at an energy of 1 MeV. This simulation was performed only with the galactic and the Jovian electron source. The heliocentric distance and heliographic latitude of the Ulysses and Cassini trajectories are shown in the top panel.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{9069fig6.eps}\end{figure}$ Figure 5: The computed electron intensities along the Cassini (solid line) and Ulysses (dashed line) trajectories at an energy of 1 MeV. This simulation was performed with the galactic, the Jovian, and the Kronian electron sources. We set $S_{\rm j} = 1.5$ , so that the Saturn source is 1.5 times stronger than the source at Jupiter. The heliocentric distance and heliographic latitude of the Ulysses and Cassini trajectories are shown in the top panel.
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In the text

$\begin{figure} \par\includegraphics[width=5.8cm,clip]{9069fig7.eps}\vspace*{2mm} \includegraphics[width=5.8cm,clip]{9069fig8.eps}\end{figure}$ Figure 6: Contour plot of the 1 MeV electron intensity in the ecliptic plane at 1998.0 inside 10 AU: the top panel is related to the situation in Fig. 4 (no Saturn source) and the bottom panel to Fig. 5 (with Saturn source, $S_{\rm j} = 1.5$ ). The position of Ulysses is marked as the filled triangle and Cassini as the filled circle. The Parker spiral and the extensions of the Jupiter and Saturn source are clearly visible at about 5 AU and 9 AU.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{9069fig9.eps}\end{figure}$ Figure 7: The computed electron intensities along the Ulysses trajectory at an energy of 1 MeV. Displayed are simulations with three factors of $S_{\rm j}$ , 0.3, 1.5, and 7.5 (dashed lines), together with the simulation without the Saturn source ( $S_{\rm j}$ = 0, solid line). The diffusion tensor $\tens{\kappa}$ and the solar wind speed $\vec u_{\rm sw}$ are time-independent, so that the latitudinal structure of the solar wind (see Fig. 2) is kept at the conditions valid for the solar minimum. The minimum and maximum value of the solar wind velocity are set to $V_{\rm min}$ = 400 km s^-1 and $V_{\rm max}$ = 750 km s^-1. The heliocentric distance and heliographic latitude of the Ulysses trajectory are shown in the top panel.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{9069fig10.eps}\end{figure}$ Figure 8: The computed electron intensities along the Cassini trajectory at an energy of 1 MeV. Displayed are simulations with three factors of $S_{\rm j}$ , 0.3, 1.5 and 7.5 (dashed lines), together with the simulation without the Saturn source ( $S_{\rm j}$ = 0, solid line). The diffusion tensor $\tens{\kappa}$ and the solar wind speed $\vec u_{\rm sw}$ are time-independent, so that the latitudinal structure of the solar wind (see Fig. 2) is kept at the conditions valid for the solar minimum. The minimum and maximum value of the solar wind velocity are set to $V_{\rm min}$ = 400 km s^-1 and $V_{\rm max}$ = 750 km s^-1. The heliocentric distance and heliographic latitude of the Cassini trajectory are shown in the top panel.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{9069fig11.eps}\end{figure}$ Figure 9: The computed electron intensities along the Ulysses trajectory at an energy of 1 MeV, where $S_{\rm j} = 1.5$ . A time-dependent model (Lange et al. 2006) and parameters for the solar activity are used here (solid line). The beginning of the solar maximum phase is set to 1995.8, the transition period for the solar wind field to two months, and four months for the latitudinal diffusion coefficient. In comparison, the dashed lines display the result without the solar activity variation (as in Fig. 5). The heliocentric distance and heliographic latitude of the Ulysses trajectory are shown in the top panel.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{9069fig12.eps}\end{figure}$ Figure 10: The computed electron intensities along the Cassini trajectory at an energy of 1 MeV, where $S_{\rm j} = 1.5$ . A time-dependent model (Lange et al. 2006) and parameters for the solar activity are used here (solid line). The beginning of the solar maximum phase is set to 1995.8, the transition period for the solar wind field to two months and four months for the latitudinal diffusion coefficient. In comparison, the dashed lines display the result without the solar activity variation (as in Fig. 5). The heliocentric distance and heliographic latitude of the Cassini trajectory are shown in the top panel.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{9069fig1.eps}\par\includegraphics[width=6.7cm,clip]{9069fig2.eps}\end{figure}$	Figure 1: The trajectories of the Ulysses and Cassini spacecraft. Ulysses was launched in 1990 and orbits the Sun now for the third time. Shown is Ulysses´ first orbit. Cassini was launched in 1997 and reached Saturn in 2004. Source: http://helio.estec.esa.nl/ulysses/ and http://saturn.jpl.nasa.gov/home/index.cfm.
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$\begin{figure} \par\includegraphics[width=6.8cm,clip]{9069fig3.eps}\end{figure}$	Figure 2: The latitudinal structure of the solar wind velocity $f_{\rm\Theta } {v_{\rm0}}$ , see Eq. (5) for solar minimum conditions.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{9069fig5.eps}\end{figure}$	Figure 4: The computed electron intensities (normalized to the galactic source) along the Cassini (solid line) and Ulysses (dashed line) trajectories at an energy of 1 MeV. This simulation was performed only with the galactic and the Jovian electron source. The heliocentric distance and heliographic latitude of the Ulysses and Cassini trajectories are shown in the top panel.
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