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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1973fig1.eps} \end{figure}$ Figure 1: The cooling of relativistic electrons behind a strong shock ( $\chi =4$ and $\Delta u=100~{\rm km~s^{-1}}$ ). The thick solid line is the momentum distribution at the shock located at 600 R_*. The three solid lines are the distributions away from the shock, at locations 600 R_*-1.5 R_*, 600 R_*-3 R_* and 600 R_*-4.5 R_*. We assumed $N(1~{\rm MeV/c})=1$ at 600 R_* and $B_*=100~{\rm G}$ . The dashed lines indicate the momentum that the relativistic electrons must have to produce synchrotron radiation between 2 and 20 cm ( $450~{\rm MeV/c}>p>140~{\rm MeV/c}$ ).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1973fig2.eps} \end{figure}$ Figure 2: The emissivity behind a strong forward shock at r=600 R_* for 2 different wavelengths. The dashed line is the emissivity at 20 cm and the solid line at 2 cm. We normalised the emissivity to the highest value.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1973fig3.eps} \end{figure}$ Figure 3: The VLA observations (21 Dec. 1984) for Cyg OB2 No. 9 with revised error bars. The solid line represents a single shock model that explains the non-thermal radio emission. The stellar parameters are given in Table 1.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{1973fig4.eps}\includegraphics[width=8.4cm,clip]{1973fig5.eps} \end{figure}$ Figure 4: a) Left panel: the combinations of $\chi$ , $R_{\rm S}$ and B_* that fit the observations for Cyg OB2 No. 9 lie in the grey area in the figure. Projections on two planes are plotted to situate the solutions in the parameter space. b) Right panel: for all possible combinations of the model parameters that explain the radio observations of Cyg OB2 No. 9, the values for the surface magnetic field B_* and the shock velocity jump $\Delta {u}$ are shown. The solid line represents $\Delta u^3 B_*^{3/2}$ is constant.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1973fig2.eps} \end{figure}$	Figure 2: The emissivity behind a strong forward shock at r=600 R_* for 2 different wavelengths. The dashed line is the emissivity at 20 cm and the solid line at 2 cm. We normalised the emissivity to the highest value.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1973fig3.eps} \end{figure}$	Figure 3: The VLA observations (21 Dec. 1984) for Cyg OB2 No. 9 with revised error bars. The solid line represents a single shock model that explains the non-thermal radio emission. The stellar parameters are given in Table 1.
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