All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0399fig1.eps}\end{figure}$ Figure 1: Observed distribution of 1165 pulsar periods with $0.02~{\rm s}<P<8.52$ s ( upper panel) and simulated distribution corresponding to case (1) in Table 2 ( lower panel). The solid lines represent the analytical fit to the observed distribution in the form of a gamma function with m=0.28 and a=2.28, while the dashed line represents the parent density distribution gamma function with m=0.34 and a=2.52.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0399fig2.eps}\end{figure}$ Figure 2: Observed distribution of 238 pulse widths W₁₀ taken from GH96 ( upper panel) and simulated distribution corresponding to case (1) in Table 2 ( lower panel).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0399fig3.eps}\end{figure}$ Figure 3: Observed distribution of 149 magnetic inclination angles $\alpha$ taken from Rankin (1993b) ( upper panel) and simulated distribution corresponding to case (1) in Table 2 ( lower panel). The solid line represents the parent density distribution function expressed by Eq. (9).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0399fig2.eps}\end{figure}$	Figure 2: Observed distribution of 238 pulse widths W₁₀ taken from GH96 ( upper panel) and simulated distribution corresponding to case (1) in Table 2 ( lower panel).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0399fig3.eps}\end{figure}$	Figure 3: Observed distribution of 149 magnetic inclination angles $\alpha$ taken from Rankin (1993b) ( upper panel) and simulated distribution corresponding to case (1) in Table 2 ( lower panel). The solid line represents the parent density distribution function expressed by Eq. (9).
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