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The interiors of Uranus and Neptune: current understanding and open questions

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TLDR
This review focuses on the things the authors do not know about the interiors of Uranus and Neptune with a focus on why the planets may be different, rather than the same.
Abstract
Uranus and Neptune form a distinct class of planets in our Solar System. Given this fact, and ubiquity of similar-mass planets in other planetary systems, it is essential to understand their interior structure and composition. However, there are more open questions regarding these planets than answers. In this review, we concentrate on the things we do not know about the interiors of Uranus and Neptune with a focus on why the planets may be different, rather than the same. We next summarize the knowledge about the planets' internal structure and evolution. Finally, we identify the topics that should be investigated further on the theoretical front as well as required observations from space missions. This article is part of a discussion meeting issue 'Future exploration of ice giant systems'.

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Citations
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Journal ArticleDOI

Neptune and Uranus: ice or rock giants?

TL;DR: This article considers how observations of Neptune’s atmospheric temperature and composition can provide further constraints and suggests a rock giant provides a more consistent match to available atmospheric observations.
Journal ArticleDOI

Auroral emissions from Uranus and Neptune

TL;DR: Uranus and Neptune possess highly tilted/offset magnetic fields whose interaction with the solar wind shapes unique twin asymmetric, highly dynamical, magnetospheres, which radiate complex auroral emissions, both reminiscent of those observed at the other planets and unique to the ice giants as discussed by the authors.
Posted Content

Uranus and Neptune are key to understand planets with hydrogen atmospheres

TL;DR: In this paper, the atmospheric dynamics and structure of the last unexplored planets of the Solar System, including Uranus and Neptune, have been studied and the authors show that they hold crucial keys to understand the atmosphere dynamics and structures of planets with hydrogen atmospheres.
References
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Journal ArticleDOI

Origin of the orbital architecture of the giant planets of the Solar System.

TL;DR: This model reproduces all the important characteristics of the giant planets' orbits, namely their final semimajor axes, eccentricities and mutual inclinations, provided that Jupiter and Saturn crossed their 1:2 orbital resonance.
Journal ArticleDOI

The Effects of Snowlines on C/O in Planetary Atmospheres

TL;DR: In this article, the authors present a mechanism that can produce such atmospheric deviations from the stellar C/O ratio in protoplanetary disks, where different snowlines of oxygen- and carbon-rich ices, especially water and carbon monoxide, will result in systematic variations in the C /O ratio both in the gas and in the condensed phases.
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A common mass scaling for satellite systems of gaseous planets

TL;DR: It is shown that the overall properties of the satellite systems of Jupiter, Saturn and Uranus arise naturally, and it is suggested that similar processes could limit the largest moons of extrasolar Jupiter-mass planets to Moon-to-Mars size.
Journal ArticleDOI

Structure and evolution of super-Earth to super-Jupiter exoplanets - I. Heavy element enrichment in the interior

TL;DR: In this paper, the authors examine the uncertainties in current planetary models and quantify their impact on the planet cooling histories and massradius relationships, including the differences between the various equations of state used to characterize the heavy material thermodynamic properties, the distribution of heavy elements within planetary interiors, their chemical composition, and their thermal contribution to the planet evolution.
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The atmosphere of Uranus: Results of radio occultation measurements with Voyager 2

TL;DR: In this article, the authors investigated the Uranian atmosphere on the basis of S-band and X-band occultation observations (including measurements of Doppler frequency perturbations) obtained during the Voyager 2 encounter with Uranus in January 1986.
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