author={T. Guillot},
  journal={Planetary and Space Science},
  • T. Guillot
  • Published 1999
  • Physics
  • Planetary and Space Science
Abstract Interior models of Jupiter and Saturn are calculated and compared in the framework of the three-layer assumption, which rely on the perception that both planets consist of three globally homogeneous regions: a dense core, a metallic hydrogen envelope, and a molecular hydrogen envelope. Within this framework, constraints on the core mass and abundance of heavy elements (i.e. elements other than hydrogen and helium) are given by accounting for uncertainties on the measured gravitational… Expand
The Interior of Saturn
A source of uncertainty in Saturn interior models is the lack of a unique rotation rate to be ascribed to the deep (metallic-hydrogen) interior. As a result, models are not uniquely constrained byExpand
Comparative evolution of Jupiter and Saturn
Abstract We present evolutionary sequences for Jupiter and Saturn, based on new non-gray model atmospheres, which take into account the evolution of the solar luminosity and partitioning of denseExpand
The Interior Structure, Composition, and Evolution of Giant Planets
We discuss our current understanding of the interior structure and thermal evolution of giant planets. This includes the gas giants, such as Jupiter and Saturn, that are primarily composed ofExpand
Shock Compression of Deuterium and the Interiors of Jupiter and Saturn
Recently, deuterium has been the focus of a high level of experimental and theoretical activity, sparked by a disagreement on the experimental value of the maximum compression along the principalExpand
Signature of helium rain and dilute cores in Jupiter's interior from empirical equations of state
Measurements of Jupiter's gravity field by Juno have been acquired with unprecedented precision, but uncertainties in the planet’s hydrogen–helium equation of state (EOS) and the hydrogen–heliumExpand
Jupiter internal structure: the effect of different equations of state
Heavy elements, even though its smaller constituent, are crucial to understand Jupiter formation history. Interior models are used to determine the amount of heavy elements in Jupiter interior,Expand
Models and theoretical spectrum for the free oscillations of Saturn
We constructed new models of Saturn with an allowance made for a helium mass fraction of ∼0.18–0.25 in its atmosphere. Our modeling shows that the composition of Saturn differs markedly from theExpand
Jupiter’s formation and its primordial internal structure
The composition of Jupiter and the primordial distribution of the heavy elements are determined by its formation history. As a result, in order to constrain the primordial internal structure ofExpand
The phase diagram of water and the magnetic fields of Uranus and Neptune
Abstract The interior of giant planets can give valuable information on formation and evolution processes of planetary systems. However, the interior and evolution of Uranus and Neptune is stillExpand
Understanding Saturn’s interior from the Cassini Grand Finale gravity measurements
Context. Measurements of Saturn’s gravity field by Cassini Grand Finale have been acquired with high precision. It has been demonstrated that the even gravitational harmonics J6–J10 have largerExpand


Nonadiabatic Models of Jupiter and Saturn
Abstract New interior models for Jupiter and Saturn are described that do not assume the temperature profiles to be adiabatic throughout the entire hydrogen-helium envelope. These models include theExpand
Optimized Jupiter, Saturn, and Uranus interior models
We present models of Jupiter, Saturn, and Uranus which exactly match recent accurate determinations of these planets' gravitational harmonics. The models are computed to third order in the rotationalExpand
New Constraints on the Composition of Jupiter from Galileo Measurements and Interior Models
Abstract Using the helium abundance measured by Galileo in the atmosphere of Jupiter and interior models reproducing the observed external gravitational field, we derive new constraints on theExpand
Comparative evolution of Jupiter and Saturn
Abstract We present evolutionary sequences for Jupiter and Saturn, based on new non-gray model atmospheres, which take into account the evolution of the solar luminosity and partitioning of denseExpand
Are the Giant Planets Fully Convective
Abstract All current models of internal structure and evolution of the giant planets assume a convective and adiabatic stratification. The purpose of this work is to reexamine this hypothesis usingExpand
Structure and Transport in the Solar Nebula from Constraints on Deuterium Enrichment and Giant Planets Formation
Abstract A simplified analytical model of an evolutionary nebula is used to generate temperature–density radial profiles following the procedure elaborated by Dubrulle ( Icarus 106 , 59, 1993). EachExpand
Chemical Models of the Deep Atmospheres of Jupiter and Saturn
New and updated chemical kinetic data, elemental abundances, and thermodynamic data are used for thermochemical equilibrium and, where relevant, thermochemical kinetic calculations of gas abundancesExpand
Thermal structure and heat balance of the outer planets
Current knowledge of the thermal structure and energy balance of the outer planets is summarized. The Voyager spacecraft experiments have provided extensive new information on the atmosphericExpand
The helium abundance of Saturn from Voyager measurements
Voyager radio-occultation and IR spectroscopy measurements are combined to infer an He mole fraction in the upper troposphere of Uranus of 0.152 + or - 0.033; the corresponding mass fraction is Y =Expand
Liquid metallic hydrogen and the structure of brown dwarfs and giant planets
Electron-degenerate, pressure-ionized hydrogen (usually referred to as metallic hydrogen) is the principal constituent of brown dwarfs, the long-sought objects which lie in the mass range between theExpand