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Title:
Planet formation
Authors:
Lissauer, Jack J.
Affiliation:
AA(New York State University, Stony Brook; California Univ., Santa Barbara)
Publication:
In: Annual review of astronomy and astrophysics. Vol. 31 (A94-12726 02-90), p. 129-174. (Annual Reviews Homepage)
Publication Date:
00/1993
Category:
Lunar and Planetary Exploration
Origin:
STI
NASA/STI Keywords:
Planetary Evolution, Planetary Systems, Solar System Evolution, Terrestrial Planets, Orbital Mechanics, Planetology
DOI:
10.1146/annurev.aa.31.090193.001021
Bibliographic Code:
1993ARA&A..31..129L

Abstract

Models of planetary formation are developed using the present single example of a planetary system, supplemented by limited astrophysical observations of star-forming regions and circumstellar disks. The solar nebula theory and the planetesimal hypothesis are discussed. The latter is found to provide a viable theory of the growth of the terrestrial planets, the cores of the giant planets, and the smaller bodies present in the solar system. The formation of solid bodies of planetary size should be a common event, at least around young stars which do not have binary companions orbiting at planetary distances. Stochastic impacts of large bodies provide sufficient angular momentum to produce the obliquities of the planets. The masses and bulk compositions of the planets can be understood in a gross sense as resulting from planetary growth within a disk whose temperature and surface density decreased with distance from the growing sun.

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