Astronomy & Astrophysics

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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2730_f1.ps}\end{figure}$ Figure 1: Collimated outflow model. A cold, dense (density n_b^*) plasma cloud ejected from an AGN moves along the magnetic field lines and runs into interstellar/intergalactic gas clouds (density $n_{\rm i}^\ast \ll n_b^\ast$ ) with an ultra-relativistic speed.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{2730_f2.ps}\end{figure}$ Figure 2: Maximal transmission coefficient as a function of resonant pitch-angle cosine at $\mu_j\leq V_{\rm A}/\tilde{V}$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{2730_f3.ps}\end{figure}$ Figure 3: Total particle density (solid curves) and wave-energy density (dashed curves) as a function of position for $V_{\rm A}/\tilde{V}=0.01$ , $\alpha _3=1$ , and three values of $\Delta U/U_0$ (from left to right) of 10⁴, 100, and 1. The position is measured in asymptotic mean free paths (see Eq. (48)).
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In the text

$\begin{figure} \par\includegraphics[width=17.5cm,clip]{2730_f4.ps}\end{figure}$ Figure 4: Gamma radiation from a relativistic outflow with n_b=10⁹ cm^-3, R=10¹⁴ cm, d=10¹³ cm and $\Gamma (t=0)=300$ propagating into a medium with $n_{\rm i}^\ast = 0.1$ cm^-3 and B=5 G viewed at an aspect angle of $0.1^\circ$ and t=1 h observer's time. The bulk Lorentz factor at that time is indicated in each panel. The components shown result from $\pi ^0$ -decay (solid curves), positron annihilation (dashed curves) and bremsstrahlung (dot-dashed curves). The left-hand and right-hand panels show the results for the original model of Pohl & Schlickeiser (2000) and for the present model, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{2730_fb.ps}\end{figure}$ Figure B.1: Wave spectrum generated by protons (or electrons) as a function of resonant pitch-angle cosine for $V_{\rm A}/\tilde{V}=0.1$ and $T_j=\alpha_1~4\tilde{V}V_{\rm A}/(\tilde{V}+V_{\rm A})^2$ with $\alpha _1=1.0$ (solid curve), 1.15 (dashed curve), and 1.25(dot-dashed curve). Note that the area under each curve is proportional to the wave-energy density.

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2730_f1.ps}\end{figure}$	Figure 1: Collimated outflow model. A cold, dense (density n_b^*) plasma cloud ejected from an AGN moves along the magnetic field lines and runs into interstellar/intergalactic gas clouds (density $n_{\rm i}^\ast \ll n_b^\ast$ ) with an ultra-relativistic speed.
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$\begin{figure} \par\includegraphics[width=7.9cm,clip]{2730_f2.ps}\end{figure}$	Figure 2: Maximal transmission coefficient as a function of resonant pitch-angle cosine at $\mu_j\leq V_{\rm A}/\tilde{V}$ .
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$\begin{figure} \par\includegraphics[width=7.4cm,clip]{2730_f3.ps}\end{figure}$	Figure 3: Total particle density (solid curves) and wave-energy density (dashed curves) as a function of position for $V_{\rm A}/\tilde{V}=0.01$ , $\alpha _3=1$ , and three values of $\Delta U/U_0$ (from left to right) of 10⁴, 100, and 1. The position is measured in asymptotic mean free paths (see Eq. (48)).
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