All Figures

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{6856fig1.eps} \end{figure}$ Figure 1: Dynamic radio spectrum recorded by the radio spectralpolarimeter (Mann et al. 1992) of the Astrophysical Institute Potsdam. It shows an example of a solar type II radio burst. Further explanations are given in Sect. 1.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{6856fig2.ps} \end{figure}$ Figure 2: Behavior of the fluxes of energetic electrons (0.1-0.4 MeV) and protons (0.8-1.0 MeV), the solar wind speed $V_{\rm SW}$ , the proton temperature, the proton number density, and the magnitude of the magnetic field ( from top to bottom) during the crossing of a CIR by Ulysses (Scholer et al. 1999).
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{6856fig3.eps} \end{figure}$ Figure 3: Sketch of the shock configuration. Both the in-flowing toward the shock front and out-flowing protons (" ${\bf p}$ '') and electrons (" ${\bf e}$ '') move along the upstream magnetic field lines ( ${\vec B}^{\rm up}$ ). The shock moves along the shock normal ( ${\vec n}$ ). The excited whistler waves (denoted with their wave vector ${\vec k}$ ) propagate away from the shock along the magnetic field lines, which is chosen to be the positive direction.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{6856fig4.eps} \end{figure}$ Figure 4: Dispersion relation for the LCP (dashed line) Alfvén and RCP (solid line) whistler wave for S = 20. Both propagate along the ambient magnetic field.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{6856fig5.eps} \end{figure}$ Figure 5: Solution of the resonance curve, Eq. (22), for S=20 and $\omega ' = 0.166$ (dashed) and 0.211 (solid line) in the $(\beta _{\parallel }^{\rm e},\beta _{\perp }^{\rm e})$ -plane. The dashed-dotted line corresponds to a pitch angle of 45 $^{\circ }$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{6856fig6.eps} \end{figure}$ Figure 6: Relation between $\beta _{\perp }^{\rm e}$ and the kinetic energy $W_{\rm kin}/m_{\rm e}c^{2}$ , Eq. (23), where $\vert\beta _{\parallel }^{\rm e}\vert=0.076$ and $\beta _{\perp }^{\rm e}$ takes the values along the dotted line in Fig. 5.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{6856fig1.eps} \end{figure}$	Figure 1: Dynamic radio spectrum recorded by the radio spectralpolarimeter (Mann et al. 1992) of the Astrophysical Institute Potsdam. It shows an example of a solar type II radio burst. Further explanations are given in Sect. 1.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{6856fig2.ps} \end{figure}$	Figure 2: Behavior of the fluxes of energetic electrons (0.1-0.4 MeV) and protons (0.8-1.0 MeV), the solar wind speed $V_{\rm SW}$ , the proton temperature, the proton number density, and the magnitude of the magnetic field ( from top to bottom) during the crossing of a CIR by Ulysses (Scholer et al. 1999).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{6856fig4.eps} \end{figure}$	Figure 4: Dispersion relation for the LCP (dashed line) Alfvén and RCP (solid line) whistler wave for S = 20. Both propagate along the ambient magnetic field.
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$\begin{figure} \par\includegraphics[width=8.1cm,clip]{6856fig5.eps} \end{figure}$	Figure 5: Solution of the resonance curve, Eq. (22), for S=20 and $\omega ' = 0.166$ (dashed) and 0.211 (solid line) in the $(\beta _{\parallel }^{\rm e},\beta _{\perp }^{\rm e})$ -plane. The dashed-dotted line corresponds to a pitch angle of 45 $^{\circ }$ .
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{6856fig6.eps} \end{figure}$	Figure 6: Relation between $\beta _{\perp }^{\rm e}$ and the kinetic energy $W_{\rm kin}/m_{\rm e}c^{2}$ , Eq. (23), where $\vert\beta _{\parallel }^{\rm e}\vert=0.076$ and $\beta _{\perp }^{\rm e}$ takes the values along the dotted line in Fig. 5.
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