All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0207fig1.eps} \end{figure}$ Figure 1: Variation of $\displaystyle \frac{\sigma}{\sigma_{\rm C}}$ with height for the quiet Sun model of Vernazza et al. (1981) for different B₀: 1) 10 G; 2) 100 G and 3) 1000 G.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0207fig2.eps} \end{figure}$ Figure 2: Variation of $\displaystyle \left. \frac{\tilde{\tau}_{\rm Joule}}{\tilde{\tau}_{\rm visc}} \right\vert _{{\rm A.w.} ({\parallel}) \atop {\rm f.ms.w.}s ({\parallel})}$ with height in the low solar atmosphere (Vernazza et al. 1981) for different B₀: 1) 5 G; 2) 10 G; 3) 100 G; and 4) 1000 G.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0207fig3.eps} \end{figure}$ Figure 3: Variation of $\displaystyle \left. \frac{\tilde{\tau}_{\rm frict}}{\tilde{\tau}_{\rm visc}} \right\vert _{ {\rm s.w.} ({\parallel})}$ with height in the solar chromosphere (Vernazza et al. 1981).
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In the text

$\begin{figure} \par\includegraphics[width=18cm,clip]{0207fig4.eps} \end{figure}$ Figure 4: Typical values of the collisional and viscous damping time ratios for parallel propagating a) Alfvén and fast magnetoacoustic waves $\displaystyle \left. \frac{\tilde{\tau}_{\rm Joule}}{\tilde{\tau}_{\rm visc}} \right\vert _{{\rm A.w.} ({\parallel}) \atop {\rm f.ms.w.} ({\parallel})}$ and b) acoustic wave $\displaystyle \left. \frac{\tilde{\tau}_{\rm frict}}{\tilde{\tau}_{\rm visc}} \right\vert _{ {\rm s.w.} ({\parallel})}$ in the prominence plasma for $B_0 = 10 ~\mbox{G}$ and $\displaystyle \frac{n_{\rm n}}{n} = 1$ .
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In the text

$\begin{figure} \par\includegraphics[width=18cm,clip]{0207fig5.eps} \end{figure}$ Figure 5: Typical values of the collisional and viscous damping time ratios for propagating across the magnetic field a) fast magnetoacoustic $\displaystyle \left. \frac{\tilde{\tau}_{\rm Joule}}{\tilde{\tau}_{\rm visc}} \right\vert _{ {\rm f.ms.w.} ({\perp})}$ and b) acoustic $\displaystyle \left. \frac{\tilde{\tau}_{\rm frict}}{\tilde{\tau}_{\rm visc}} \right\vert _{{\rm s.w.} ({\perp})}$ wave in the prominence plasma for $B_0 = 10 ~\mbox{G}$ and $\displaystyle \frac{n_{\rm n}}{n} = 1$ .
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{0207fig6.eps} \end{figure}$ Figure 6: a) Critical frequency of the Alfvén and fast magnetoacoustic waves versus height in the low solar atmosphere for different B₀: 1) $1000~\mbox{G}$ , 2) $100~\mbox{G}$ , 3) $10~\mbox{G}$ . b) Critical frequency of the acoustic wave versus height in the low solar atmosphere for 1) longitudinal ( $\parallel$ ) and 2) transverse ( $\perp$ ) propagation of waves. c) The range of values of critical frequency of the Alfvén and fast magnetoacoustic waves in the prominence plasma for $B_0 = 10 ~\mbox{G}$ and $\displaystyle \frac{n_{\rm n}}{n} = 1$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0207fig1.eps} \end{figure}$	Figure 1: Variation of $\displaystyle \frac{\sigma}{\sigma_{\rm C}}$ with height for the quiet Sun model of Vernazza et al. (1981) for different B₀: 1) 10 G; 2) 100 G and 3) 1000 G.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0207fig2.eps} \end{figure}$	Figure 2: Variation of $\displaystyle \left. \frac{\tilde{\tau}_{\rm Joule}}{\tilde{\tau}_{\rm visc}} \right\vert _{{\rm A.w.} ({\parallel}) \atop {\rm f.ms.w.}s ({\parallel})}$ with height in the low solar atmosphere (Vernazza et al. 1981) for different B₀: 1) 5 G; 2) 10 G; 3) 100 G; and 4) 1000 G.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0207fig3.eps} \end{figure}$	Figure 3: Variation of $\displaystyle \left. \frac{\tilde{\tau}_{\rm frict}}{\tilde{\tau}_{\rm visc}} \right\vert _{ {\rm s.w.} ({\parallel})}$ with height in the solar chromosphere (Vernazza et al. 1981).
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