$\begin{figure} \par\includegraphics[width=8.5cm,clip]{6328fig1.eps} \end{figure}$ Figure 1: Inner bremsstrahlung photon spectrum per neutron calculated numerically from the expressions given in Petrosian & Ramaty (1972) (solid line). Also shown for comparison is the approximate fit (1) (dashed line) but the difference between the two curves is very small in this energy range, mostly $\ll$ $10\%$ , so that they can barely be discriminated visually.
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{6328fig2.eps} \end{figure}$ Figure 2: Geometry for calculation of X-ray halo brightness as a function of angle to the Earth-Sun direction.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{6328fig3.eps} \end{figure}$ Figure 3: $I(\epsilon ,\theta )/i(\epsilon )$ , as a function of the angle $\theta$ between the line of sight and the Earth-Sun direction.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{6328fig1.eps} \end{figure}$	Figure 1: Inner bremsstrahlung photon spectrum per neutron calculated numerically from the expressions given in Petrosian & Ramaty (1972) (solid line). Also shown for comparison is the approximate fit (1) (dashed line) but the difference between the two curves is very small in this energy range, mostly $\ll$ $10\%$ , so that they can barely be discriminated visually.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{6328fig2.eps} \end{figure}$	Figure 2: Geometry for calculation of X-ray halo brightness as a function of angle to the Earth-Sun direction.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{6328fig3.eps} \end{figure}$	Figure 3: $I(\epsilon ,\theta )/i(\epsilon )$ , as a function of the angle $\theta$ between the line of sight and the Earth-Sun direction.
Open with DEXTER