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Figure 1: Scenario I at 20 000 years after the start of giant planet migration, showing the mass, inclination and eccentricity of objects. Small black dots represent super-planetesimals; white filled circles are rocky protoplanets; grey filled circles are icy protoplanets and the large highlighted grey filled circle is the giant. The dotted line in the upper panel shows the eccentricity at which the pericentre of an exterior object intersects the orbit of the giant. The location of the 2:1, 3:2 and 4:3 resonances with the giant are indicated. |
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Figure 2: Scenario I at 100 000 years after the start of giant planet migration. The giant has now moved inward to 2.68 AU and has scattered a significant amount of mass into exterior orbits. |
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Figure 3: Scenario I at 160 000 years after the start of giant planet migration. The giant has now moved inward to 0.52 AU. The scattered exterior disk has grown, but a substantial amount of mass in planetesimals and six rapidly accreting protoplanets remain interior to the giant. The outer three of these six are in first order resonances with the giant. |
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Figure 4:
Detail of the interior regions of Scenario I at 160 000 years
after the start of giant planet migration, showing e vs. a for
objects ![]() ![]() ![]() ![]() ![]() |
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Figure 5:
Scenario I at 170 000 years after the start of giant planet
migration. The giant has now stopped at 0.1 AU. All interior mass has
accreted into a single ![]() ![]() |
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Figure 6:
Surface density evolution ( left hand panel) and accretion rates
( right hand panel) for Scenario I. Growing surface density peaks at the 2:1 and 3:2 resonances sweep through the inner system ahead of the giant.
Accretion rates increase after ![]() |
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Figure 7: Interior and exterior surviving solids as a percentage of initial disk mass at 170 000 years. |
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Figure 8: Comparison of computer generated interior planets with the interior regions of four known "hot Neptune'' systems. |
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Figure 9:
Scenario I: collision of the inner planet with the central
star as the giant moves inward to 0.05 AU. Resonant angles for the
2:1 resonance are read on the left hand axis: light grey symbols
plot the angle
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Figure 10:
Scenario IV: survival of the inner planet as the giant moves
inward to 0.05 AU. Resonant angles for the 2:1 resonance are read on
the left hand axis: light grey symbols
plot the angle
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Figure 11: Number and total mass of protoplanets predicted in the habitable zone assuming orbital re-circularization with conservation of angular momentum. |
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