All Figures

$\begin{figure} \par\includegraphics[width=8.8cm]{4833fig1.eps}\end{figure}$ Figure 1: The far downstream cross-helicity $H_{\rm c,2}$ as a function of Alfvénic Mach number M for different shock proper speeds $u_1 = V_1 \Gamma _1$ . $M_{\rm c} = \sqrt {r}$ is the critical Mach number, below which the downstream Alfvén speed exceeds the local plasma speed, and the shock becomes non-evolutionary. The spectral index of the turbulence power-spectrum is q=1.5
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{4833fig2.eps}\end{figure}$ Figure 2: Form of the flow profile ( upper panel) and the local cross helicity across the shock when $M/M_{\rm c} = 2$ ( lower panel). Shock proper speeds u₁ range from 0.1 c to 10 c (lines from bottom to top, respectively). In the upper panel the flow speed is in arbitrary units, showing only the form of the transition from far upstream speed V₁ to that of the downstream, V₂, and the spatial range across which the transition takes place for both the flow speed and the cross-helicities. See text for details.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{4833fig3.eps} \end{figure}$ Figure 3: Ratio of the scattering centre compression ratio r_k to that of the gas r for different shock proper speeds u₁ as functions of the Alvénic Mach number M. Lines are drawn for upstream cross-helicity $H_{\rm c1} = -1$ (group of the uppermost lines) and +1 (lower group). The spectral index of the turbulence power spectrum is q=1.5 and $M_{\rm c} = \sqrt {r}$ ; see text for details.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{4833fig4.eps} \end{figure}$ Figure 4: Same as Fig. 3, but for $H_{\rm c1} = -0$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{4833fig5.eps} \end{figure}$ Figure 5: Sketch of the scattering-centre compression ratio as a function of wavenumber ( left) and the resulting accelerated particle spectrum ( right) in a thick relativistic shock. L denotes the shock thickness.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{4833fig1.eps}\end{figure}$	Figure 1: The far downstream cross-helicity $H_{\rm c,2}$ as a function of Alfvénic Mach number M for different shock proper speeds $u_1 = V_1 \Gamma _1$ . $M_{\rm c} = \sqrt {r}$ is the critical Mach number, below which the downstream Alfvén speed exceeds the local plasma speed, and the shock becomes non-evolutionary. The spectral index of the turbulence power-spectrum is q=1.5
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$\begin{figure} \par\includegraphics[width=8.8cm]{4833fig3.eps} \end{figure}$	Figure 3: Ratio of the scattering centre compression ratio r_k to that of the gas r for different shock proper speeds u₁ as functions of the Alvénic Mach number M. Lines are drawn for upstream cross-helicity $H_{\rm c1} = -1$ (group of the uppermost lines) and +1 (lower group). The spectral index of the turbulence power spectrum is q=1.5 and $M_{\rm c} = \sqrt {r}$ ; see text for details.
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$\begin{figure} \par\includegraphics[width=8.8cm]{4833fig4.eps} \end{figure}$	Figure 4: Same as Fig. 3, but for $H_{\rm c1} = -0$ .
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$\begin{figure} \par\includegraphics[width=8.8cm]{4833fig5.eps} \end{figure}$	Figure 5: Sketch of the scattering-centre compression ratio as a function of wavenumber ( left) and the resulting accelerated particle spectrum ( right) in a thick relativistic shock. L denotes the shock thickness.
Open with DEXTER