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$\begin{figure} \par\resizebox{8cm}{!}{\includegraphics[clip]{H4706f1.ps}} \end{figure}$ Figure 1: Comparison of dust temperature profiles obtained with different methods for a BE sphere with central density $n({\rm H}_2)=4.4\times 10^6$ cm^-3, gas temperature $T_{\rm g}=12$ K, and radius R=0.1 pc. The solid and dotted curves shows the result obtained with the ray integration method of ZWG and the Monte Carlo code, without including the effects of re-emission. The two results are in excellent agreement. The short-dashed curve shows the dust temperature computed with the Monte Carlo code including re-emission. In all three cases the cloud has no envelope.
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In the text

$\begin{figure} \par\resizebox{8cm}{!}{\includegraphics[clip]{H4706f2.ps}} \end{figure}$ Figure 2: Dust temperature profiles (including re-emission) for the cloud model shown in Fig. 1 for different choices of the dust opacity: solid curve, OH1; dotted curve, OH4; short-dashed curve, OH5; long-dashed curve, OH8 (see text for the definitions). The gas-to-dust ratio was varied so that the total extinction at 2.2 $\mu$ m is the same in all cases. The cloud is embedded in a spherical outer envelope with total extinction $A_{2.2~\mu\rm{m}}^{\rm env} = 0.1$ .
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In the text

$\begin{figure} \par\resizebox{8cm}{!}{\includegraphics[angle=270,clip]{H4706f3.ps}} \end{figure}$ Figure 3: The top panel shows the dust temperature ( top half) and density distribution ( bottom half) of a singular isothermal toroid with H₀=0.5, seen edge-on. The density on the boundary is $n({\rm H}_2)=10^4$ cm^-3 and the isopycnic curves are logarithmically spaced by 0.5. The density distribution is azimuthally symmetric and also symmetric with respect to the midplane. The maximum outer temperature is 15 K and the isothermal curves are spaced by 1 K. The bottom panel shows the emission at 1.3 mm ( top half) and at 350 $\mu$ m ( bottom half). The isophotal curves are logarithmically spaced by 0.2 starting from the lower value $0.01\times I_\nu ^{\rm max}$ . With the adopted opacity law (OH5), the peak values are $I_\nu ^{\rm max} =77$ MJy sr^-1 at 1.3 mm and 382 MJy sr^-1at 350 $\mu$ m (in this and in the following figures, the maps have not been convolved with an observing beam).
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In the text

$\begin{figure} \par\resizebox{8cm}{!}{\includegraphics[angle=270,clip]{H4706f4.ps}} \end{figure}$ Figure 4: Model results for a spherical (Bonnor-Ebert) cloud core heated by the standard ISRF and a B3 star located at 0.15 pc from the surface of the cloud (on the left side in this figure). The core has central density $n({\rm H}_2)=4.4\times 10^6$ cm^-3, gas temperature $T_{\rm g}=10$ K, and radius R=0.1 pc. The top panel shows the dust temperature ( top half) and the density ( bottom half). Isopycnic curves are logarithmically spaced by 0.5 and the boundary density is $n({\rm H}_2)=2.3\times 10^3$ cm^-3. Isothermal curves are spaced by 2 K starting from $T_{\rm d}=14$ K. The middle and bottom panels show the emission at 1.3 mm, 350 $\mu$ m, 100 $\mu$ m and 60 $\mu$ m. Isophotes are logarithmically spaced by 0.2 starting from $0.01\times I_\nu ^{\rm max}$ . The peak intensity $I_\nu ^{\rm max}$ is 78 MJy sr^-1 at 1.3 mm, 3347 MJy sr^-1 at 350 $\mu$ m, 1404 MJy sr^-1 at 100 $\mu$ m and 200 MJy sr^-1 at 60 $\mu$ m.
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In the text

$\begin{figure} \par\resizebox{14cm}{!}{\includegraphics[angle=270,clip]{H4706f5.ps}} \end{figure}$ Figure 5: Density and temperature distribution in the magnetic 3-D model. Panels on the left (right) side show results in the y=0 (z=0) plane, respectively. The top panels show the gas density, with isopycnic curves logarithmically spaced by 0.5, and density on the boundary $n({\rm H}_2)=10^4$ cm^-3. The middle panels shows the dust temperature distribution, with isothermal curves spaced by 1 K between the minimum (7 K) and maximum (14 K) values. The bottom panels shows the gas temperature, with isothermal levels ranging from 7 to 14 K.
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In the text

$\begin{figure} \par\resizebox{8cm}{!}{\includegraphics[angle=270,clip]{H4706f6.ps}} \end{figure}$ Figure 6: Normalized emission for the 3-D model, seen edge-on (top panel) and face-on (bottom panel). Each panel shows the emission at 1.3 mm (top half) and at 350 $\mu$ m (bottom half). Isophotal curves are logarithmically spaced by 0.2 starting from the lower value $0.01\times I_\nu ^{\rm max}$ . With the adopted opacity law (OH5), the peak values are: $I_\nu ^{\rm max}=89$ MJy sr^-1 at 1.3 mm and 460 MJy sr^-1 at 350 $\mu$ m (edge-on case); $I_\nu ^{\rm max} =72$ MJy sr^-1 at 1.3 mm and 307 MJy sr^-1 at 350 $\mu$ m (face-on case).
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In the text