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The fate of volatiles within Jupiter’s Circumplanetary Disk

Presentation #509.02 in the session Icy Moons Interior and Ice Shell (Oral Presentation)

Published onOct 23, 2023
The fate of volatiles within Jupiter’s Circumplanetary Disk

At the very end of its growth, Jupiter became surrounded by a circumplanetary disk (CPD) composed of gas and dust, where the Galilean moons formed. How the moon formed and interacted with the CPD remains an outstanding question. It has been proposed that the formation of their building blocks was triggered by streaming instability and their growth via pebble accretion. Once formed, the moons underwent Type I and Type II migration by interacting with the disk’s gas. In the early stages of the CPD, the migration of satellesimals occurred over so short timescales that most bodies fell onto Jupiter, suggesting that the Galilean moons formed later during the CPD evolution. Other studies suggest that the moons sequentially formed and migrated inward. This suggests that the moons were trapped in mean motion resonances, halting their migration. In the coming years, the ESA mission JUICE and NASA mission Europa-Clipper will study Jupiter’s Icy moons composition.

In this context we aim at studying the volatiles and their snowlines in a two-dimensional CPD, to establish a connection between the moon bulk compositions and the origin of their building blocks. We developed a 2D quasi-stationary CPD, whose thermal profile is computed from a Grey Atmosphere radiative transfer model. This model considers viscous heating, accretion heating, and heating of the upper layers of the CPD by Jupiter. A volatile transport module has been coupled to our model, allowing us to study the evolution of volatiles ices and vapors in the vicinity of their icelines. after Jupiter’s formation.

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