Deuterated water and the formation of the satellites of Uranus

Abstract

The satellites of Uranus orbit in a low-eccentricity, equatorial plane that is tilted by 98 degrees relative to the solar system -- a geometry that mirrors Uranus's extreme axial tilt. Although a giant impact could have tipped Uranus, how the satellites came to share this orientation remains uncertain. Proposed formation pathways include primordial accretion followed by reorientation, formation from debris generated by the tilting impact, and reaccretion from a massive ring produced by the tidal disruption of passing bodies from the outer solar system. Current observations do not discriminate among these scenarios. Using the James Webb Space Telescope, we measured the deuterium-to-hydrogen (D/H) ration in the water ice of the five regular satellites of Uranus. We find an average D/H ratio of $2.1\pm 0.2\times 10^{-4}$, nearly five times higher than that of Uranus and comparable to the values measured in comets. This enrichment is inconsistent with with any formation scenario in which substantial Uranian material was incorporated into the satellites, thereby excluding models that require significant mixing in an impact-derived vapor disk. The observed D/H ratios are instead compatible with models in which the satellites accreted from material that remained largely separate from Uranus, such as debris from a disrupted pre-existing satellite system or from a tidally captured outer solar system body. The innermost regular satellite, Miranda, exhibits a marginally elevated D/H ratio (2.8 $\sigma$ above the average of the other satellites), potentially indicating a distinct formation history or source of water and offering an important clue for distinguishing amount competing models.

arXiv commentThis is the author's version of the manuscript that has been published in the Proceedings of the National Academy of Sciences, including corrections from the published version

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