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The recently observed population of 540 free-floating Jupiter-mass objects, including 40 dynamically soft pairs, and two triples, in the Trapezium cluster have raised interesting questions on their formation and evolution. We test various scenarios for the origin and survivability of these free floating Jupiter-mass objects and Jupiter-mass Binary Objects (JuMBOs) in the Trapezium cluster. The numerical calculations are performed by direct N N -body integration of the stars and planets in the Trapezium cluster starting with a wide variety of planets in various configurations. We discuss four models: SPP 𝒮𝒫𝒫, in which selected stars have two outer orbiting Jupiter-mass planets; SPM 𝒮𝒫ℳ, where selected stars are orbited by Jupiter-mass planet-moon pairs; ISF ℐ𝒮ℱ in which JuMBOs form in situ with the stars, and FFC ℱℱ𝒞, where we introduce a population of free-floating single Jupiter-mass objects, but no initialised binaries. Models FFC ℱℱ𝒞 and SPP 𝒮𝒫𝒫 fail to produce enough JuMBOs. Models SPM 𝒮𝒫ℳ can produce sufficient free-floaters and JuMBOs, but requires unusually wide orbits for the planet-moon system around the star. The observed JuMBOs and free-floating Jupiter-mass objects in the Trapezium cluster are best reproduced if they formed in pairs and as free-floaters together with the other stars in a smooth (Plummer) density profile with a virial radius of 0. 5 ∼0. 5 pc. A fractal (with fractal dimension 1. 6) stellar density distribution also works, but requires relatively recent formations (⪆ 0. 2 ⪆0. 2 Myr after the other stars formed) or a high (⪆ 50 ⪆50 %) initial binary fraction. This would make the primordial binary fraction of JuMBOs even higher than the already large observation fraction of 8 ∼8 % (42/540). The fraction of JuMBOs will continue to drop with time, and the lack of JuMBOs in Upper Scorpius could then result in its higher age, causing more JuMBOs to be ionized. We then also predict that the interstellar density of Jupiter-mass objects (mostly singles with some 2 ∼2 % lucky surviving binaries) is 0. 05 ∼0. 05 per pc ^-3 −3 (or around 0. 24 per star).
Zwart et al. (Tue,) studied this question.