Astronomy & Astrophysics

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$\begin{figure} \par\includegraphics[width=8cm,clip]{1115fig1.eps} \end{figure}$ Figure 1: The very early R-band ( $\nu_{R}=4.6\times 10^{14}~{\rm Hz}$ ) light curve powered by the mildly magnetized outflow (the degrees of the magnetization have been marked in the figure) interacting with the interstellar medium. The parameters taken in the calculation are: z=1, $E_{\rm kin}=10^{53}~{\rm erg}$ , $L=2\times 10^{51}~{\rm erg~s^{-1}}$ , $\eta =300$ , $n_1=1~{\rm cm^{-3}}$ , $\epsilon _{\rm e}=0.3$ and the radiation efficiency $\epsilon =\epsilon _{\rm e}$ . For $\sigma =0$ and the forward shock, it is assumed that $\epsilon _{\rm B}=0.01$ .
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1115fig2.eps} \end{figure}$ Figure 2: The very early R-band light curve powered by the mildly magnetized outflow (the degree of the magnetization has been marked in the figure) interacting with the stellar wind. The parameters taken here are the same to those of Fig. 1 except $n_1=3\times 10^{35}R^{-2}~{\rm cm^{-3}}$ .
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1115fig3.eps} \end{figure}$ Figure 3: Coordinates used in the calculation of the polarization properties of a slab of mixed field (after Laing 1980).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1115fig2.eps} \end{figure}$	Figure 2: The very early R-band light curve powered by the mildly magnetized outflow (the degree of the magnetization has been marked in the figure) interacting with the stellar wind. The parameters taken here are the same to those of Fig. 1 except $n_1=3\times 10^{35}R^{-2}~{\rm cm^{-3}}$ .
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$\begin{figure} \par\includegraphics[width=8cm,clip]{1115fig3.eps} \end{figure}$	Figure 3: Coordinates used in the calculation of the polarization properties of a slab of mixed field (after Laing 1980).
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