Fig. 8
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Two models with high α = 0.02 and high Z = 0.02, giving the same dust mass as in the nominal model, but with half the gas mass. This may represent either an initially higher metallicity or a gradual gas loss to disc winds. The lower migration rates make it possible to form Jupiter analogues both at δ = 3 × 10−5 (top) and at δ = 10−4 (bottom).
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