Interiors of giant planets inside and outside the solar system.

@article{Guillot1999InteriorsOG,
  title={Interiors of giant planets inside and outside the solar system.},
  author={Tristan Guillot},
  journal={Science},
  year={1999},
  volume={286 5437},
  pages={
          72-7
        }
}
  • T. Guillot
  • Published 1 October 1999
  • Physics, Geology
  • Science
An understanding of the structure and composition of the giant planets is rapidly evolving because of (i) high-pressure experiments with the ability to study metallic hydrogen and define the properties of its equation of state and (ii) spectroscopic and in situ measurements made by telescopes and satellites that allow an accurate determination of the chemical composition of the deep atmospheres of the giant planets. However, the total amount of heavy elements that Jupiter, Saturn, Uranus, and… 
10.13 – Giant Planets
The Formation of Uranus and Neptune among Jupiter and Saturn
The outer giant planets, Uranus and Neptune, pose a challenge to theories of planet formation. They exist in a region of the solar system where long dynamical timescales and a low primordial density
Extrasolar Planets: From clouds to planet systems: formation and evolution of stars and planets
The discovery of more than hundred extrasolar planet candidates challenges our understanding of star and planet formation. Do we have to modify the theories that were mostly developed for the solar
MASS–RADIUS RELATIONSHIPS FOR VERY LOW MASS GASEOUS PLANETS
Recently, the Kepler spacecraft has detected a sizable aggregate of objects, characterized by giant-planet-like radii and modest levels of stellar irradiation. With the exception of a handful of
SOLUBILITY OF IRON IN METALLIC HYDROGEN AND STABILITY OF DENSE CORES IN GIANT PLANETS
The formation of the giant planets in our solar system, and likely a majority of giant exoplanets, is most commonly explained by the accretion of nebular hydrogen and helium onto a large core of
Outlook: Testing Planet Formation Theories
The discovery of the first planetary companion to a solar-type star by Mayor and Queloz (1995) launched the extrasolar planetary systems era. Observational and theoretical progress in this area has
Formation, Orbital and Internal Evolutions of Young Planetary Systems
The growing body of observational data on extrasolar planets and protoplanetary disks has stimulated intense research on planet formation and evolution in the past few years. The extremely diverse,
Synthetic evolution tracks of giant planets
Giant planet evolution models play a crucial role in interpreting observations and constraining formation pathways. However, the simulations can be slow or prohibitively difficult. To address this
Giant Planets
We review the interior structure and evolution of Jupiter, Saturn, Uranus and Neptune, and giant exoplanets with particular emphasis on constraining their global composition. Compared to the first
DYNAMICAL MEASUREMENTS OF THE INTERIOR STRUCTURE OF EXOPLANETS
Giant gaseous planets often reside on orbits in sufficient proximity to their host stars for the planetary quadrupole gravitational field to become non-negligible. In presence of an additional
...
...

References

SHOWING 1-10 OF 53 REFERENCES
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 the
Orbital migration of the planetary companion of 51 Pegasi to its present location
THE recent discovery1 and confirmation2 of a possible planetary companion orbiting the solar-type star 51 Pegasi represent a breakthrough in the search for extrasolar planetary systems. Analysis of
Interiors of the Giant Planets
From our position as inhabitants of a rather insignificant rock orbiting close in to the Sun, there is an inevitable tendency to think of the giant planets (Jupiter, Saturn, Uranus, and Neptune) as
Orbital Evolution of Planets Embedded in a Planetesimal Disk
The existence of the Oort comet cloud, the Kuiper belt, and plausible inefficiencies in planetary core formation all suggest that there was once a residual planetesimal disk of mass ∼10–100 M⊕ in the
DETECTION OF EXTRASOLAR GIANT PLANETS
▪ Abstract Eight extrasolar planet candidates have now been identified, all revealed by Keplerian Doppler shifts in their host stars. The masses (m sin i) lie between 0.5 and 7 MJUP, and the
Chemical Equilibrium Abundances in Brown Dwarf and Extrasolar Giant Planet Atmospheres
We explore detailed chemical equilibrium abundance profiles for a variety of brown dwarf and extrasolar giant planet atmosphere models, focusing in particular on Gl 229B, and derive the systematics
Extrasolar Giant Planets under Strong Stellar Irradiation
We investigate irradiation of extrasolar giant planets (EGPs) by treating the radiative transfer in detail, so that the flux from the parent star interacts with all relevant depths of the planetary
...
...