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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0540fig1.ps} \end{figure}$ Figure 1: Deuterium enrichment factor f calculated at the epochs of the condensation of water for the minimum mass and maximum mass solar nebula models derived from Mousis et al. (2000). The vertical bold solid lines correspond to the range of values of f inferred in the icy solids produced in Jupiter and Saturn's feeding zones.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0540fig2.ps} \end{figure}$ Figure 2: Mass distribution in the Jovian subnebula described by Paper II, for various values of t in years. The Jovian subnebula is characterized by the parameters $M_{\rm D}=0.001~M_{\rm Jup}$ , $R_{\rm D}=704~R_{\rm Jup}$ , and $\alpha = 0.0004$ . The time t=0 corresponds to the epoch when the formation of Jupiter was completed. Dashed curves represent the zone of the subnebula where T and P are high enough to vaporize H₂O ice. Plain curves correspond to the zone of the subnebula where T and P conditions are low enough to preserve H₂O ice from evaporation. With time, the cold zone expands inward.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0540fig1.ps} \end{figure}$	Figure 1: Deuterium enrichment factor f calculated at the epochs of the condensation of water for the minimum mass and maximum mass solar nebula models derived from Mousis et al. (2000). The vertical bold solid lines correspond to the range of values of f inferred in the icy solids produced in Jupiter and Saturn's feeding zones.
Open with DEXTER