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The Institute of Physics (IOP) is a leading scientific society promoting physics and bringing physicists together for the benefit of all. It has a worldwide membership of around 50 000 comprising physicists from all sectors, as well as those with an interest in physics. It works to advance physics research, application and education; and engages with policy makers and the public to develop awareness and understanding of physics. Its publishing company, IOP Publishing, is a world leader in professional scientific communications. A publishing partnership. Models of the dynamical evolution of the early solar system that follow the dispersal of the gaseous protoplanetary disk have been widely successful in reconstructing the current orbital configuration of the giant planets.

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Statistically, some of the most successful dynamical evolution simulations have initially included a hypothetical fifth giant planet, of ice giant (IG) mass, which gets ejected by a gas giant during the early solar system's proposed instability phase. We investigate the likelihood of an IG ejection (IGE) event by either Jupiter or Saturn through constraints imposed by the current orbits of their wide-separation regular satellites Callisto and Iapetus, respectively. We show that planetary encounters that are sufficient to eject an IG often provide excessive perturbations to the orbits of Callisto and Iapetus, making it difficult to reconcile a planet ejection event with the current orbit of either satellite. Quantitatively, we compute the likelihood of reconciling a regular Jovian satellite orbit with the current orbit of Callisto following an IGE by Jupiter of ~42%, and conclude that such a large likelihood supports the hypothesis of a fifth giant planet's existence.

A similar calculation for Iapetus reveals that it is much more difficult for Saturn to have ejected an IG and reconciled a Kronian satellite orbit with that of Iapetus (likelihood ~1%), although uncertainties regarding the formation of Iapetus, with its unusual orbit, complicates the interpretation of this result. Export citation and abstract. Various solar system formation models argue that the giant planets underwent planetesimal driven migration (e.g., Fernandez & Ip; Malhotra; Hahn & Malhotra; Tsiganis et al.

) at early times ( 1 Gyr) following a dynamical instability. The Nice model, originally presented by Gomes et al. (), Morbidelli et al. (), and Tsiganis et al. (), with subsequent variants under the same name, has been the most successful in reproducing the settling of the four giant planets into their present orbital configuration (Tsiganis et al.; Morbidelli et al.; Levison et al. ), the Late Heavy Bombardment at ~700 Myr (Gomes et al.

), the capture of Jupiter's Trojan asteroids (Morbidelli et al. Balam pichkari video. ), the capture of gas giant irregular satellites (Nesvorný et al.

), as well as the structure of the Kuiper Belt (Levison et al. ) and how its dynamical evolution led to the contamination of the outer asteroid belt by primitive trans-Neptunian objects (Levison et al. The precise nature of giant planet migration in the early solar system remains uncertain due to our lack of knowledge regarding each body's initial conditions following their formation out of the solar nebula and the chaotic nature of the migration process.