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$\begin{figure} \par\resizebox{8cm}{!}{\includegraphics{Gf232_f1.eps}} \par\end{figure}$ Figure 1: The path length of $\gamma$ -rays a) and range of electrons b) as a function of energy in molecular hydrogen. The $\gamma$ -ray data is taken from the compilation of Cullen et al. (1989) and the electron data from Berger & Seltzer (1964).
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In the text

$\begin{figure} \resizebox{8.8cm}{!}{\includegraphics[clip]{Gf232_f2.eps}} \end{figure}$ Figure 2: The surface density, $\Sigma$ , as a function of height above the midplane, H, in astronomical units (AUs) for two models with normalising values, $\Sigma _{0}$ and exponent n, with $\Sigma _{0} = 4250$ g cm^-2 and n = -1.0 (solid line) and $\Sigma _{0} = 1700$ g cm^-2 and n = -1.5 (dashed line)and for three radial distances of a) 1 AU, b) 3 AU and c) 5 AU. The diamonds and squares give path lengths of 150 and 300 g cm^-2measured from the top of the nebula.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{Gf232_f3.eps}\par\end{figure}$ Figure 3: a) The number of $\gamma$ -rays that Compton scatter and and the number of positive ions as a function of path length in H₂ for an incident flux of 10¹³ photons m^-2 (i). The number of electrons as a function of path length taking into account the ionization loss of 10 g cm^-2 (ii) and also including a retarding electric field of 1 V m^-1 (iii). b) The charge excess as a function of path length for the ionization loss (solid line) and also including the retarding electric field (broken line). The model used is for r = 3 AU and $\Sigma _{0} = 4250$ g cm^-2 with n = -1.0.
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In the text

$\begin{figure} \par\resizebox{8cm}{!}{\includegraphics{Gf232_f1.eps}} \par\end{figure}$	Figure 1: The path length of $\gamma$ -rays a) and range of electrons b) as a function of energy in molecular hydrogen. The $\gamma$ -ray data is taken from the compilation of Cullen et al. (1989) and the electron data from Berger & Seltzer (1964).
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