Yupiter Planetasi Turali Mlmet

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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. ), 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.

However, Morbidelli et al. () argued that smooth divergent migration of the gas giants is unable to sufficiently excite their orbital eccentricities and inclinations to their observed values. Additionally, Brasser et al.

() showed that such migration from an initial resonant configuration following the dispersal of the gaseous disk leads to excessive orbital eccentricities in the previously formed terrestrial bodies via sweeping secular resonances. A proposed solution, known as the jumping-Jupiter scenario (Brasser et al. ), invokes close encounters between the gas giants and an ice giant (IG), resulting in the step-wise migration of Jupiter and Saturn from their initial mean-motion resonance. Tom clancy s the division cracked. This can sufficiently excite giant planet eccentricities and inclinations while jumping over the problematic secular frequencies of the terrestrial planets. In addition, the jumping-Jupiter scenario does not disrupt the asteroid belt's observed morphology (Morbidelli et al.

A statistical study by Nesvorný () of the dynamical evolution of the solar system during such a phase of frequent planetary encounters showed that the likelihood of reconstructing the current orbital configuration of the four giant planets is increased when a fifth giant planet of approximately Uranian mass is included in the early solar system. The instability, which gives rise to multiple planetary encounters, results in the ejection of the hypothetical fifth giant planet, reconstructing the outer solar system while preserving the orbits of the inner terrestrial bodies over long timescales (Batygin et al.; Nesvorný & Morbidelli ). Such planet scattering events (Rasio & Ford; Weidenschilling & Marzari ), applicable to any multi-body system, provide a potential explanation for the existence of the recently detected 'free-floating' planets (e.g., Delorme et al.; Liu et al.; Luhman & Esplin ).

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