The Interiors of Uranus and Neptune: Current Understanding and Open Questions
arXiv:2007.10783 · doi:10.1098/rsta.2019.0474
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.
Accepted for publication in Philosophical Transactions of the Royal Society A
References in corpus (16)
- Comparing Jupiter interior structure models to Juno gravity measurements and the role of a dilute core
- New models of Jupiter in the context of Juno and Galileo
- Saturn Ring Seismology: Evidence for Stable Stratification in the Deep Interior of Saturn
- Condensation-inhibited convection in hydrogen-rich atmospheres: Stability against double-diffusive processes and thermal profiles for Jupiter, Saturn, Uranus, and Neptune
- Methane on Uranus: The case for a compact CH4 cloud layer at low latitudes and a severe CH4 depletion at high-latitudes based on re-analysis of Voyager occultation measurements and STIS spectroscopy
- Deep Atmosphere Composition, Structure, Origin, and Exploration, with Particular Focus on Critical in situ Science at the Icy Giants
- An Exploration of Double Diffusive Convection in Jupiter as a Result of Hydrogen-Helium Phase Separation
- The Formation of Uranus & Neptune: Challenges and Implications For Intermediate-Mass Exoplanets
- Effect of Non-Adiabatic Thermal Profiles on the Inferred Compositions of Uranus and Neptune
- Thermal evolution of Uranus and Neptune I: adiabatic models
- Properties of hydrogen, helium, and silicon dioxide mixtures in giant planet interiors
- Uranian Satellite Formation by Evolution of a Water Vapor Disk Generated by a Giant Impact
- Orbits and resonances of the regular moons of Neptune
- Convective storms and atmospheric vertical structure in Uranus and Neptune
- Time-Series Analysis of Broadband Photometry of Neptune from K2
- Saturn's rings as a seismograph to probe Saturn's internal structure
Cited by in corpus (19)
- Diamond formation from hydrocarbon mixtures in planets
- Empirical Structure Models of Uranus and Neptune
- Revising the Giant Planet Mass-Metallicity Relation: Deciphering the Formation Sequence of Giant Planets
- Planet Mass and Metallicity: The Exoplanets and Solar System Connection
- Ariel Planetary Interiors White Paper
- Could Uranus and Neptune form by collisions of planetary embryos?
- Searching for gravitational waves via Doppler tracking by future missions to Uranus and Neptune
- Zonal winds of Uranus and Neptune: Gravitational harmonics, dynamic self-gravity, shape, and rotation
- The deep oxygen abundance in Solar System Giant Planets, with a new derivation for Saturn
- One EURO for Uranus: the Elliptical Uranian Relativity Orbiter mission
- Linking Uranus' temperature profile to wind-induced magnetic fields
- Planetary albedo is limited by the above-cloud atmosphere: Implications for sub-Neptune climate
- Prospects for a local detection of dark matter with future missions to Uranus and Neptune
- The linear-mixing approximation in silica-water mixtures at planetary conditions
- Thermal evolution of Uranus and Neptune II -- Deep thermal boundary layer
- Possible in situ formation of Uranus and Neptune via Pebble Accretion
- A Denser Hydrogen Inferred from First-Principles Simulations Challenges Jupiter's Interior Models
- Did Uranus' regular moons form via a rocky giant impactor?
- The Arcanum Mission: Scientific Objectives and Instruments for Neptune, Triton and KBOs