$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0586fig1.eps} \end{figure}$ Figure 1: Log of grain radius (s in cm) against the log of differential spatial density (N(s) in $\rm cm^{-4}$ ) as obtained from Lamy et al. (1987) for comet Halley derived through space-craft experiments (Table 1). The dotted curve represents the best-fit polynomial equation as derived in the present work.
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In the text

$\begin{figure} \par\includegraphics[height=7.5cm,width=7.5cm,clip]{0586fig2.eps}\end{figure}$ Figure 2: The observed polarisation values of comet P/Halley at $\lambda = 0.365~\mu{\rm m}$ . The dotted curve represents the calculated values for Mie type scattering with (n, k)=(1.403,0.024).
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In the text

$\begin{figure} \par\includegraphics[height=7.5cm,width=7.5cm,clip]{0586fig3.eps} \end{figure}$ Figure 3: The observed polarisation values of comet P/Halley at $\lambda = 0.484~\mu{\rm m}$ . The dotted curve represents the calculated values for Mie type scattering with (n, k)=(1.390,0.026).
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In the text

$\begin{figure} \par\includegraphics[height=7.5cm,width=7.5cm,clip]{0586fig4.eps} \end{figure}$ Figure 4: The observed polarisation values of comet P/Halley at $\lambda = 0.684~\mu{\rm m}$ . The dotted curve represents the calculated values for Mie type scattering with (n, k)=(1.386,0.038).
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In the text

$\begin{figure} \par\includegraphics[height=7.5cm,width=7.5cm,clip]{0586fig5.eps} \end{figure}$ Figure 5: Log of perihelion distance against log (-g), where g is the relative abundance of coarser grains, as discussed in the paper. The straight line represents the equation $\log~(-g)= \log~(2.5) + {\frac 2 3}\log~(q)$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0586fig1.eps} \end{figure}$	Figure 1: Log of grain radius (s in cm) against the log of differential spatial density (N(s) in $\rm cm^{-4}$ ) as obtained from Lamy et al. (1987) for comet Halley derived through space-craft experiments (Table 1). The dotted curve represents the best-fit polynomial equation as derived in the present work.
Open with DEXTER

$\begin{figure} \par\includegraphics[height=7.5cm,width=7.5cm,clip]{0586fig2.eps}\end{figure}$	Figure 2: The observed polarisation values of comet P/Halley at $\lambda = 0.365~\mu{\rm m}$ . The dotted curve represents the calculated values for Mie type scattering with (n, k)=(1.403,0.024).
Open with DEXTER

$\begin{figure} \par\includegraphics[height=7.5cm,width=7.5cm,clip]{0586fig3.eps} \end{figure}$	Figure 3: The observed polarisation values of comet P/Halley at $\lambda = 0.484~\mu{\rm m}$ . The dotted curve represents the calculated values for Mie type scattering with (n, k)=(1.390,0.026).
Open with DEXTER

$\begin{figure} \par\includegraphics[height=7.5cm,width=7.5cm,clip]{0586fig4.eps} \end{figure}$	Figure 4: The observed polarisation values of comet P/Halley at $\lambda = 0.684~\mu{\rm m}$ . The dotted curve represents the calculated values for Mie type scattering with (n, k)=(1.386,0.038).
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$\begin{figure} \par\includegraphics[height=7.5cm,width=7.5cm,clip]{0586fig5.eps} \end{figure}$	Figure 5: Log of perihelion distance against log (-g), where g is the relative abundance of coarser grains, as discussed in the paper. The straight line represents the equation $\log~(-g)= \log~(2.5) + {\frac 2 3}\log~(q)$ .
Open with DEXTER