Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{h3705f1.eps} \end{figure}$ Figure 1: A schematic picture illustrating the integration procedure. A thin shell of electrons enclosed within the half-opening angle of the jet, $\psi _{j}$ is divided into cells, each $\delta \Omega _{j}$ thick. Each such cell contains $\delta N_\gamma$ electrons. The observer is located at the angle $\psi _{\rm obs}$ from the jet axis. Integration is performed by summation over $\theta$ contributions from cells located at different radii.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[clip]{h3705f2.eps}} \end{figure}$ Figure 2: The average spectrum of the blazar 3C 279 during the February 1996 flare. Data points are from Hartman et al. (2001). Thick, solid line shows the averaged spectrum of our model (see text for parameters). Thin lines represent various components of the spectrum.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[clip]{h3705f3.eps}} \end{figure}$ Figure 3: $\gamma$ -ray (upper panel - $\nu F_\nu$ flux at 400 MeV) and X-ray (lower panel - integrated 2-10 keV flux) light-curves of the blazar 3C 279 during the February 1996 flare. Data points are from Wehrle et al. (1998). Thick, solid line shows the light-curves of our model.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{h3705f4.eps} \end{figure}$ Figure 4: Spectral index $\alpha (F_\nu \propto \nu ^{-\alpha })$ evolution (left panels) and hardness-intensity diagram (right panels) of the blazar 3C 279 during the February 1996 flare. Upper panels show the index at 400 MeV while lower panels show the index at 6 keV.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[clip]{h3705f5.eps}} \end{figure}$ Figure 5: Evolution of the electron energy distribution during the February 1996 flare of the blazar 3C 279. Step between the curves is $\Delta r = 0.2~r_0$ .
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[clip]{h3705f2.eps}} \end{figure}$	Figure 2: The average spectrum of the blazar 3C 279 during the February 1996 flare. Data points are from Hartman et al. (2001). Thick, solid line shows the averaged spectrum of our model (see text for parameters). Thin lines represent various components of the spectrum.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[clip]{h3705f3.eps}} \end{figure}$	Figure 3: $\gamma$ -ray (upper panel - $\nu F_\nu$ flux at 400 MeV) and X-ray (lower panel - integrated 2-10 keV flux) light-curves of the blazar 3C 279 during the February 1996 flare. Data points are from Wehrle et al. (1998). Thick, solid line shows the light-curves of our model.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{h3705f4.eps} \end{figure}$	Figure 4: Spectral index $\alpha (F_\nu \propto \nu ^{-\alpha })$ evolution (left panels) and hardness-intensity diagram (right panels) of the blazar 3C 279 during the February 1996 flare. Upper panels show the index at 400 MeV while lower panels show the index at 6 keV.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[clip]{h3705f5.eps}} \end{figure}$	Figure 5: Evolution of the electron energy distribution during the February 1996 flare of the blazar 3C 279. Step between the curves is $\Delta r = 0.2~r_0$ .
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