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$\begin{figure} \par\includegraphics[width=8cm,clip]{4936fig1.eps} \end{figure}$ Figure 1: Schematic representation of the layer model of the HMF (see text).
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In the text

$\begin{figure} \par\includegraphics[width=6.7cm,clip]{4936fig2A.eps}\par\includegraphics[width=6.7cm,clip]{4936fig2B.eps} \end{figure}$ Figure 2: A) Radial dependence of the mean free paths used in the solution of the transport equation. B) Latitudinal dependence of the solar wind velocity and the radial mean free path.
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In the text

$\begin{figure} \par\includegraphics[width=6.7cm,clip]{4936fig3.eps} \end{figure}$ Figure 3: The proton spectrum obtained in this work at 1AU compared with data from IMP 8 and BESS. We used the local interstellar medium spectrum (LIS) of Webber & Lockwood (2001) as a boundary condition.
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In the text

$\begin{figure} \par\includegraphics[width=6.7cm,clip]{4936fig4.eps} \end{figure}$ Figure 4: Radial profiles of the solutions obtained from this work. Full squares (from 1 to 12 AU) correspond to spacecraft measurements in the ecliptic plane during solar minimum periods when qA >0. The outermost two (open) squares at 56 and 72 AU correspond to data taken at latitudes far from the ecliptic plane (see text).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{4936fig1.eps} \end{figure}$	Figure 1: Schematic representation of the layer model of the HMF (see text).
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$\begin{figure} \par\includegraphics[width=6.7cm,clip]{4936fig2A.eps}\par\includegraphics[width=6.7cm,clip]{4936fig2B.eps} \end{figure}$	Figure 2: A) Radial dependence of the mean free paths used in the solution of the transport equation. B) Latitudinal dependence of the solar wind velocity and the radial mean free path.
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$\begin{figure} \par\includegraphics[width=6.7cm,clip]{4936fig3.eps} \end{figure}$	Figure 3: The proton spectrum obtained in this work at 1AU compared with data from IMP 8 and BESS. We used the local interstellar medium spectrum (LIS) of Webber & Lockwood (2001) as a boundary condition.
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$\begin{figure} \par\includegraphics[width=6.7cm,clip]{4936fig4.eps} \end{figure}$	Figure 4: Radial profiles of the solutions obtained from this work. Full squares (from 1 to 12 AU) correspond to spacecraft measurements in the ecliptic plane during solar minimum periods when qA >0. The outermost two (open) squares at 56 and 72 AU correspond to data taken at latitudes far from the ecliptic plane (see text).
Open with DEXTER