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The chemistry of protoplanetary fragments formed via gravitational instabilities

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Figure

Figure 1. The evolution of the hydrodynamic simulation. The snapshots cover approximately 4000 yrs of disc evolution, through fragmentation into a numberof objects, of which four are able to resist shearing and spiral arm shocks, which we label John, Paul,
Figure 2. Mid-plane temperatures of the disc simulation at t = 2852 (left) and 3913 yrs (right), corresponding to the third and sixth panels Figure 1
Table 1. Initial gas phase fractional abundancesenergies, EX(i) = ni/n and molecular binding (desorption)b
Figure 3. Temperature (top panels) and number density (bottom panels) of the four fragments calculated from their constituent particles (see Tablevalues are shown with a solid line, while the shaded region indicates the standard deviation
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