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These planetesimals then similarly scatter off the next planet they encounter, successively moving the orbits of Uranus , Neptune , and Saturn outwards.

This process continues until the planetesimals interact with the innermost and most massive giant planet, Jupiter , whose immense gravity sends them into highly elliptical orbits or even ejects them outright from the Solar System.

This, in contrast, causes Jupiter to move slightly inward. The low rate of orbital encounters governs the rate at which planetesimals are lost from the disk, and the corresponding rate of migration.

After several hundreds of millions of years of slow, gradual migration, Jupiter and Saturn, the two inmost giant planets, cross their mutual mean-motion resonance.

This resonance increases their orbital eccentricities , destabilizing the entire planetary system. The arrangement of the giant planets alters quickly and dramatically.

These ice giants then plough into the planetesimal disk, scattering tens of thousands of planetesimals from their formerly stable orbits in the outer Solar System.

Eventually, the giant planets reach their current orbital semi-major axes , and dynamical friction with the remaining planetesimal disc damps their eccentricities and makes the orbits of Uranus and Neptune circular again.

Running dynamical models of the Solar System with different initial conditions for the simulated length of the history of the Solar System will produce the various populations of objects within the Solar System.

As the initial conditions of the model are allowed to vary, each population will be more or less numerous, and will have particular orbital properties.

Proving a model of the evolution of the early Solar System is difficult, since the evolution cannot be directly observed.

The crater record on the Moon and on the terrestrial planets is part of the main evidence for the Late Heavy Bombardment LHB : an intensification in the number of impactors, at about million years after the Solar System's formation.

In the Nice model icy planetesimals are scattered onto planet-crossing orbits when the outer disc is disrupted by Uranus and Neptune causing a sharp spike of impacts by icy objects.

The migration of outer planets also causes mean-motion and secular resonances to sweep through the inner Solar System. After Jupiter and Saturn cross the resonance their combined gravitational influence destabilizes the Trojan co-orbital region allowing existing Trojan groups in the L 4 and L 5 Lagrange points of Jupiter and Neptune to escape and new objects from the outer planetesimal disk to be captured.

When Jupiter and Saturn are near but not in resonance the location where Jupiter passes Saturn relative to their perihelia circulates slowly. If the period of this circulation falls into resonance with the period that the trojans librate the range of their librations can increase until they escape.

Primordial trojans escape and a fraction of the numerous objects from the disrupted planetesimal disk temporarily inhabit it.

A large number of planetesimals would have also been captured in Jupiter's mean motion resonances as Jupiter migrated inward.

Those that remained in a resonance with Jupiter form the Hilda family. The eccentricity of other objects declined while they were in a resonance and escaped onto stable orbits in the outer asteroid belt , at distances greater than 2.

Any original populations of irregular satellites captured by traditional mechanisms, such as drag or impacts from the accretion disks, [19] would be lost during the encounters between the planets at the time of global system instability.

A fraction of these planetesimals are captured by these planets via three-way interactions during encounters between planets.

Some irregulars may have even been exchanged between planets. The resulting irregular orbits match well with the observed populations' semimajor axes, inclinations, and eccentricities.

Triton , the largest moon of Neptune, can be explained if it was captured in a three-body interaction involving the disruption of a binary planetoid.

There were not enough interactions between Jupiter and the other planets to explain Jupiter's retinue of irregulars in the initial Nice model simulations that reproduced other aspects of the outer Solar System.

This suggests either that a second mechanism was at work for that planet, or that the early simulations did not reproduce the evolution of the giant planets orbits.

The migration of the outer planets is also necessary to account for the existence and properties of the Solar System 's outermost regions. Neptune's high eccentricity causes its mean-motion resonances to overlap and orbits in the region between Neptune and its mean motion resonances to become chaotic.

The orbits of objects between Neptune and the edge of the planetesimal disk at this time can evolve outward onto stable low-eccentricity orbits within this region.

When Neptune's eccentricity is damped by dynamical friction they become trapped on these orbits. These objects form a dynamically-cold belt, since their inclinations remain small during the short time they interact with Neptune.

Later, as Neptune migrates outward on a low eccentricity orbit, objects that have been scattered outward are captured into its resonances and can have their eccentricities decline and their inclinations increase due to the Kozai mechanism , allowing them to escape onto stable higher-inclination orbits.

Other objects remain captured in resonance, forming the plutinos and other resonant populations. These two population are dynamically hot, with higher inclinations and eccentricities; due to their being scattered outward and the longer period these objects interact with Neptune.

This evolution of Neptune's orbit produces both resonant and non-resonant populations, an outer edge at Neptune's resonance, and a small mass relative to the original planetesimal disk.

The excess of low-inclination plutinos in other models is avoided due to Neptune being scattered outward, leaving its resonance beyond the original edge of the planetesimal disk.

The differing initial locations, with the cold classical objects originating primarily from the outer disk, and capture processes, offer explanations for the bi-modal inclination distribution and its correlation with compositions.

It predicts a greater average eccentricity in classical Kuiper belt object orbits than is observed 0. It also cannot explain the apparent complete absence of gray objects in the cold population, although it has been suggested that color differences arise in part from surface evolution processes rather than entirely from differences in primordial composition.

The shortage of the lowest-eccentricity objects predicted in the Nice model may indicate that the cold population formed in situ. Asian teen with big boobs and a smooth shaven pussy gets fingered.

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