Interiors of Giant Planets Inside and Outside the Solar System

• Published in: Science (American Association for the Advancement of Science) Vol. 286; no. 5437; pp. 72 - 77
• Main Author: Guillot, Tristan
• Format: Journal Article
• Language: English
• Published: United States American Society for the Advancement of Science 01.10.1999; American Association for the Advancement of Science; The American Association for the Advancement of Science
• Subjects: Astronomical Phenomena; Astronomy; Astrophysics; Atmosphere; Average linear density; Chemical composition; Evolution, Planetary; Extraterrestrial Environment; Gas giants; Grade Point Average; Heavy elements; Helium; Hydrogen; Jupiter; Metals, Heavy; Observations; Planetary orbits; Planets; Pressure; Reviews; Saturn; Scientific Concepts; Solar System; Space life sciences; Temperature; Universe; United States
• ISSN: 0036-8075; 1095-9203
• DOI: 10.1126/science.286.5437.72

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 Neptune contain remains poorly constrained. The discovery of extrasolar giant planets with masses ranging from that of Saturn to a few times the mass of Jupiter opens up new possibilities for understanding planet composition and formation. Evolutionary models predict that gaseous extrasolar giant planets should have a variety of atmospheric temperatures and chemical compositions, but the radii are estimated to be close to that of Jupiter (between 0.9 and 1.7 Jupiter radii), provided that they contain mostly hydrogen and helium.